---
_id: '13470'
abstract:
- lang: eng
text: "Context. Massive Wolf–Rayet (WR) stars dominate the radiative and mechanical
energy budget of galaxies and probe a critical phase in the evolution of massive
stars prior to core collapse. It is not known whether core He-burning WR stars
(classical WR; cWR) form predominantly through wind stripping (w-WR) or binary
stripping (b-WR). Whereas spectroscopy of WR binaries has so-far largely been
avoided because of its complexity, our study focuses on the 44 WR binaries and
binary candidates of the Large Magellanic Cloud (LMC; metallicity Z ≈ 0.5 Z⊙),
which were identified on the basis of radial velocity variations, composite spectra,
or high X-ray luminosities.\r\n\r\nAims. Relying on a diverse spectroscopic database,
we aim to derive the physical and orbital parameters of our targets, confronting
evolution models of evolved massive stars at subsolar metallicity and constraining
the impact of binary interaction in forming these stars.\r\n\r\nMethods. Spectroscopy
was performed using the Potsdam Wolf–Rayet (PoWR) code and cross-correlation techniques.
Disentanglement was performed using the code Spectangular or the shift-and-add
algorithm. Evolutionary status was interpreted using the Binary Population and
Spectral Synthesis (BPASS) code, exploring binary interaction and chemically homogeneous
evolution.\r\n\r\nResults. Among our sample, 28/44 objects show composite spectra
and are analyzed as such. An additional five targets show periodically moving
WR primaries but no detected companions (SB1); two (BAT99 99 and 112) are potential
WR + compact-object candidates owing to their high X-ray luminosities. We cannot
confirm the binary nature of the remaining 11 candidates. About two-thirds of
the WN components in binaries are identified as cWR, and one-third as hydrogen-burning
WR stars. We establish metallicity-dependent mass-loss recipes, which broadly
agree with those recently derived for single WN stars, and in which so-called
WN3/O3 stars are clear outliers. We estimate that 45 ± 30% of the cWR stars
in our sample have interacted with a companion via mass transfer. However, only
≈12 ± 7% of the cWR stars in our sample naively appear to have formed purely
owing to stripping via a companion (12% b-WR). Assuming that apparently single
WR stars truly formed as single stars, this comprises ≈4% of the whole LMC WN
population, which is about ten times less than expected. No obvious differences
in the properties of single and binary WN stars, whose luminosities extend down
to log L ≈ 5.2 [L⊙], are apparent. With the exception of a few systems (BAT99
19, 49, and 103), the equatorial rotational velocities of the OB-type companions
are moderate (veq ≲ 250 km s−1) and challenge standard formalisms of angular-momentum
accretion. For most objects, chemically homogeneous evolution can be rejected
for the secondary, but not for the WR progenitor.\r\n\r\nConclusions. No obvious
dichotomy in the locations of apparently single and binary WN stars on the Hertzsprung-Russell
diagram is apparent. According to commonly used stellar evolution models (BPASS,
Geneva), most apparently single WN stars could not have formed as single stars,
implying that they were stripped by an undetected companion. Otherwise, it must
follow that pre-WR mass-loss/mixing (e.g., during the red supergiant phase) are
strongly underestimated in standard stellar evolution models."
article_number: A151
article_processing_charge: No
article_type: original
author:
- first_name: T.
full_name: Shenar, T.
last_name: Shenar
- first_name: D. P.
full_name: Sablowski, D. P.
last_name: Sablowski
- first_name: R.
full_name: Hainich, R.
last_name: Hainich
- first_name: H.
full_name: Todt, H.
last_name: Todt
- first_name: A. F. J.
full_name: Moffat, A. F. J.
last_name: Moffat
- first_name: L. M.
full_name: Oskinova, L. M.
last_name: Oskinova
- first_name: V.
full_name: Ramachandran, V.
last_name: Ramachandran
- first_name: H.
full_name: Sana, H.
last_name: Sana
- first_name: A. A. C.
full_name: Sander, A. A. C.
last_name: Sander
- first_name: O.
full_name: Schnurr, O.
last_name: Schnurr
- first_name: N.
full_name: St-Louis, N.
last_name: St-Louis
- first_name: D.
full_name: Vanbeveren, D.
last_name: Vanbeveren
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: W.-R.
full_name: Hamann, W.-R.
last_name: Hamann
citation:
ama: Shenar T, Sablowski DP, Hainich R, et al. The Wolf–Rayet binaries of the nitrogen
sequence in the Large Magellanic Cloud. Astronomy & Astrophysics. 2019;627.
doi:10.1051/0004-6361/201935684
apa: Shenar, T., Sablowski, D. P., Hainich, R., Todt, H., Moffat, A. F. J., Oskinova,
L. M., … Hamann, W.-R. (2019). The Wolf–Rayet binaries of the nitrogen sequence
in the Large Magellanic Cloud. Astronomy & Astrophysics. EDP Sciences.
https://doi.org/10.1051/0004-6361/201935684
chicago: Shenar, T., D. P. Sablowski, R. Hainich, H. Todt, A. F. J. Moffat, L. M.
Oskinova, V. Ramachandran, et al. “The Wolf–Rayet Binaries of the Nitrogen Sequence
in the Large Magellanic Cloud.” Astronomy & Astrophysics. EDP Sciences,
2019. https://doi.org/10.1051/0004-6361/201935684.
ieee: T. Shenar et al., “The Wolf–Rayet binaries of the nitrogen sequence
in the Large Magellanic Cloud,” Astronomy & Astrophysics, vol. 627.
EDP Sciences, 2019.
ista: Shenar T, Sablowski DP, Hainich R, Todt H, Moffat AFJ, Oskinova LM, Ramachandran
V, Sana H, Sander AAC, Schnurr O, St-Louis N, Vanbeveren D, Götberg YLL, Hamann
W-R. 2019. The Wolf–Rayet binaries of the nitrogen sequence in the Large Magellanic
Cloud. Astronomy & Astrophysics. 627, A151.
mla: Shenar, T., et al. “The Wolf–Rayet Binaries of the Nitrogen Sequence in the
Large Magellanic Cloud.” Astronomy & Astrophysics, vol. 627, A151,
EDP Sciences, 2019, doi:10.1051/0004-6361/201935684.
short: T. Shenar, D.P. Sablowski, R. Hainich, H. Todt, A.F.J. Moffat, L.M. Oskinova,
V. Ramachandran, H. Sana, A.A.C. Sander, O. Schnurr, N. St-Louis, D. Vanbeveren,
Y.L.L. Götberg, W.-R. Hamann, Astronomy & Astrophysics 627 (2019).
date_created: 2023-08-03T10:14:09Z
date_published: 2019-07-16T00:00:00Z
date_updated: 2023-08-09T12:29:58Z
day: '16'
doi: 10.1051/0004-6361/201935684
extern: '1'
intvolume: ' 627'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1051/0004-6361/201935684
month: '07'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
related_material:
link:
- relation: erratum
url: https://doi.org/10.1051/0004-6361/201935684e
scopus_import: '1'
status: public
title: The Wolf–Rayet binaries of the nitrogen sequence in the Large Magellanic Cloud
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 627
year: '2019'
...
---
_id: '13471'
abstract:
- lang: eng
text: We perform an extensive numerical study of the evolution of massive binary
systems to predict the peculiar velocities that stars obtain when their companion
collapses and disrupts the system. Our aim is to (i) identify which predictions
are robust against model uncertainties and assess their implications, (ii) investigate
which physical processes leave a clear imprint and may therefore be constrained
observationally, and (iii) provide a suite of publicly available model predictions
to allow for the use of kinematic constraints from the Gaia mission. We find that
22+26−8% of all massive binary systems merge prior to the first core-collapse
in the system. Of the remainder, 86+11−9% become unbound because of the core-collapse.
Remarkably, this rarely produces runaway stars (observationally defined as stars
with velocities above 30 km s−1). These are outnumbered by more than an order
of magnitude by slower unbound companions, or “walkaway stars”. This is a robust
outcome of our simulations and is due to the reversal of the mass ratio prior
to the explosion and widening of the orbit, as we show analytically and numerically.
For stars more massive than 15 M⊙, we estimate that 10+5−8% are walkaways and
only 0.5+1.0−0.4% are runaways, nearly all of which have accreted mass from their
companion. Our findings are consistent with earlier studies; however, the low
runaway fraction we find is in tension with observed fractions of about 10%. Thus,
astrometric data on presently single massive stars can potentially constrain the
physics of massive binary evolution. Finally, we show that the high end of the
mass distributions of runaway stars is very sensitive to the assumed black hole
natal kicks, and we propose this as a potentially stringent test for the explosion
mechanism. We also discuss companions remaining bound that can evolve into X-ray
and gravitational wave sources.
article_number: A66
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: M.
full_name: Renzo, M.
last_name: Renzo
- first_name: E.
full_name: Zapartas, E.
last_name: Zapartas
- first_name: S. E.
full_name: de Mink, S. E.
last_name: de Mink
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: S.
full_name: Justham, S.
last_name: Justham
- first_name: R. J.
full_name: Farmer, R. J.
last_name: Farmer
- first_name: R. G.
full_name: Izzard, R. G.
last_name: Izzard
- first_name: S.
full_name: Toonen, S.
last_name: Toonen
- first_name: H.
full_name: Sana, H.
last_name: Sana
citation:
ama: Renzo M, Zapartas E, de Mink SE, et al. Massive runaway and walkaway stars.
Astronomy & Astrophysics. 2019;624. doi:10.1051/0004-6361/201833297
apa: Renzo, M., Zapartas, E., de Mink, S. E., Götberg, Y. L. L., Justham, S., Farmer,
R. J., … Sana, H. (2019). Massive runaway and walkaway stars. Astronomy &
Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201833297
chicago: Renzo, M., E. Zapartas, S. E. de Mink, Ylva Louise Linsdotter Götberg,
S. Justham, R. J. Farmer, R. G. Izzard, S. Toonen, and H. Sana. “Massive Runaway
and Walkaway Stars.” Astronomy & Astrophysics. EDP Sciences, 2019.
https://doi.org/10.1051/0004-6361/201833297.
ieee: M. Renzo et al., “Massive runaway and walkaway stars,” Astronomy
& Astrophysics, vol. 624. EDP Sciences, 2019.
ista: Renzo M, Zapartas E, de Mink SE, Götberg YLL, Justham S, Farmer RJ, Izzard
RG, Toonen S, Sana H. 2019. Massive runaway and walkaway stars. Astronomy &
Astrophysics. 624, A66.
mla: Renzo, M., et al. “Massive Runaway and Walkaway Stars.” Astronomy &
Astrophysics, vol. 624, A66, EDP Sciences, 2019, doi:10.1051/0004-6361/201833297.
short: M. Renzo, E. Zapartas, S.E. de Mink, Y.L.L. Götberg, S. Justham, R.J. Farmer,
R.G. Izzard, S. Toonen, H. Sana, Astronomy & Astrophysics 624 (2019).
date_created: 2023-08-03T10:14:18Z
date_published: 2019-04-11T00:00:00Z
date_updated: 2023-08-09T12:26:08Z
day: '11'
doi: 10.1051/0004-6361/201833297
extern: '1'
external_id:
arxiv:
- '1804.09164'
intvolume: ' 624'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1051/0004-6361/201833297
month: '04'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: Massive runaway and walkaway stars
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 624
year: '2019'
...
---
_id: '13472'
abstract:
- lang: eng
text: Massive stars in binaries can give rise to extreme phenomena such as X-ray
binaries and gravitational wave sources after one or both stars end their lives
as core-collapse supernovae. Stars in close orbit around a stellar or compact
companion are expected to explode as “stripped-envelope supernovae”, showing no
(Type Ib/c) or little (Type IIb) signs of hydrogen in the spectra, because hydrogen-rich
progenitors are too large to fit. The physical processes responsible for the stripping
process and the fate of the companion are still very poorly understood. Aiming
to find new clues, we investigate Cas A, which is a very young (∼340 yr) and near
(∼3.4 kpc) remnant of a core-collapse supernova. Cas A has been subject to several
searches for possible companions, all unsuccessfully. We present new measurements
of the proper motions and photometry of stars in the vicinity based on deep HST
ACS/WFC and WFC3-IR data. We identify stellar sources that are close enough in
projection but using their proper motions we show that none are compatible with
being at the location of center at the time of explosion, in agreement with earlier
findings. Our photometric measurements allow us to place much deeper (order-of-magnitude)
upper limits on the brightness of possible undetected companions. We systematically
compare them with model predictions for a wide variety of scenarios. We can confidently
rule out the presence of any stellar companion of any reasonable mass and age
(main sequence, pre main sequence or stripped) ruling out what many considered
to be likely evolutionary scenarios for Type IIb supernova (SN IIb). More exotic
scenarios that predict the presence of a compact companion (white dwarf, neutron
star or black hole) are still possible as well as scenarios where the progenitor
of Cas A was single at the moment of explosion (either because it was truly single,
or resulted from a binary that was disrupted, or from a binary merger). The presence
of a compact companion would imply that Cas A is of interest to study exotic outcomes
of binary evolution. The single-at-death solution would still require fine-tuning
of the process that removed most of the envelope through a mass-loss mechanism
yet to be identified. We discuss how future constraints from Gaia and even deeper
photometric studies may help to place further constraints.
article_number: A34
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Wolfgang E.
full_name: Kerzendorf, Wolfgang E.
last_name: Kerzendorf
- first_name: Tuan
full_name: Do, Tuan
last_name: Do
- first_name: Selma E.
full_name: de Mink, Selma E.
last_name: de Mink
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: Dan
full_name: Milisavljevic, Dan
last_name: Milisavljevic
- first_name: Emmanouil
full_name: Zapartas, Emmanouil
last_name: Zapartas
- first_name: Mathieu
full_name: Renzo, Mathieu
last_name: Renzo
- first_name: Stephen
full_name: Justham, Stephen
last_name: Justham
- first_name: Philipp
full_name: Podsiadlowski, Philipp
last_name: Podsiadlowski
- first_name: Robert A.
full_name: Fesen, Robert A.
last_name: Fesen
citation:
ama: Kerzendorf WE, Do T, de Mink SE, et al. No surviving non-compact stellar companion
to Cassiopeia A. Astronomy & Astrophysics. 2019;623. doi:10.1051/0004-6361/201732206
apa: Kerzendorf, W. E., Do, T., de Mink, S. E., Götberg, Y. L. L., Milisavljevic,
D., Zapartas, E., … Fesen, R. A. (2019). No surviving non-compact stellar companion
to Cassiopeia A. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201732206
chicago: Kerzendorf, Wolfgang E., Tuan Do, Selma E. de Mink, Ylva Louise Linsdotter
Götberg, Dan Milisavljevic, Emmanouil Zapartas, Mathieu Renzo, Stephen Justham,
Philipp Podsiadlowski, and Robert A. Fesen. “No Surviving Non-Compact Stellar
Companion to Cassiopeia A.” Astronomy & Astrophysics. EDP Sciences,
2019. https://doi.org/10.1051/0004-6361/201732206.
ieee: W. E. Kerzendorf et al., “No surviving non-compact stellar companion
to Cassiopeia A,” Astronomy & Astrophysics, vol. 623. EDP Sciences,
2019.
ista: Kerzendorf WE, Do T, de Mink SE, Götberg YLL, Milisavljevic D, Zapartas E,
Renzo M, Justham S, Podsiadlowski P, Fesen RA. 2019. No surviving non-compact
stellar companion to Cassiopeia A. Astronomy & Astrophysics. 623, A34.
mla: Kerzendorf, Wolfgang E., et al. “No Surviving Non-Compact Stellar Companion
to Cassiopeia A.” Astronomy & Astrophysics, vol. 623, A34, EDP Sciences,
2019, doi:10.1051/0004-6361/201732206.
short: W.E. Kerzendorf, T. Do, S.E. de Mink, Y.L.L. Götberg, D. Milisavljevic, E.
Zapartas, M. Renzo, S. Justham, P. Podsiadlowski, R.A. Fesen, Astronomy &
Astrophysics 623 (2019).
date_created: 2023-08-03T10:14:27Z
date_published: 2019-03-27T00:00:00Z
date_updated: 2023-08-09T12:28:17Z
day: '27'
doi: 10.1051/0004-6361/201732206
extern: '1'
external_id:
arxiv:
- '1711.00055'
intvolume: ' 623'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1051/0004-6361/201732206
month: '03'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: No surviving non-compact stellar companion to Cassiopeia A
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 623
year: '2019'
...
---
OA_place: publisher
OA_type: hybrid
_id: '6756'
abstract:
- lang: eng
text: "We study the topology generated by the temperature fluctuations of the cosmic
microwave background (CMB) radiation, as quantified by the number of components
and holes, formally given by the Betti numbers, in the growing excursion sets.
We compare CMB maps observed by the Planck satellite with a thousand simulated
maps generated according to the ΛCDM paradigm with Gaussian distributed fluctuations.
The comparison is multi-scale, being performed on a sequence of degraded maps
with mean pixel separation ranging from 0.05 to 7.33°. The survey of the CMB over
\U0001D54A2 is incomplete due to obfuscation effects by bright point sources and
other extended foreground objects like our own galaxy. To deal with such situations,
where analysis in the presence of “masks” is of importance, we introduce the concept
of relative homology. The parametric χ2-test shows differences between observations
and simulations, yielding p-values at percent to less than permil levels roughly
between 2 and 7°, with the difference in the number of components and holes peaking
at more than 3σ sporadically at these scales. The highest observed deviation between
the observations and simulations for b0 and b1 is approximately between 3σ and
4σ at scales of 3–7°. There are reports of mildly unusual behaviour of the Euler
characteristic at 3.66° in the literature, computed from independent measurements
of the CMB temperature fluctuations by Planck’s predecessor, the Wilkinson Microwave
Anisotropy Probe (WMAP) satellite. The mildly anomalous behaviour of the Euler
characteristic is phenomenologically related to the strongly anomalous behaviour
of components and holes, or the zeroth and first Betti numbers, respectively.
Further, since these topological descriptors show consistent anomalous behaviour
over independent measurements of Planck and WMAP, instrumental and systematic
errors may be an unlikely source. These are also the scales at which the observed
maps exhibit low variance compared to the simulations, and approximately the range
of scales at which the power spectrum exhibits a dip with respect to the theoretical
model. Non-parametric tests show even stronger differences at almost all scales.
Crucially, Gaussian simulations based on power-spectrum matching the characteristics
of the observed dipped power spectrum are not able to resolve the anomaly. Understanding
the origin of the anomalies in the CMB, whether cosmological in nature or arising
due to late-time effects, is an extremely challenging task. Regardless, beyond
the trivial possibility that this may still be a manifestation of an extreme Gaussian
case, these observations, along with the super-horizon scales involved, may motivate
the study of primordial non-Gaussianity. Alternative scenarios worth exploring
may be models with non-trivial topology, including topological defect models."
acknowledgement: 'PP is grateful to Julian Borill from the Planck consortium for providing
the data, and for the illuminating discussions and inputs. PP also thanks Hans Kristen
Eriksen, Anne Ducout, and Francois R. Bouchet for significantly helpful discussions
at various stages. The authors collectively thank the anonymous referee for the
invaluable comments and suggestions that have added significant value to the contents
of the manuscript. PP and RA acknowledge the support of ERC advanced grant Understanding
Random Systems through Algebraic Topology (URSAT) (no: 320422, PI: RA). This work
is also part of a project that has received funding for PP and TB from the European
Research Council (ERC) under the European Union’s Horizon 2020 research and innovation
programme (grant agreement ERC advanced grant 740021– Advances in Research on THeories
of the dark UniverSe (ARTHUS), PI: TB). HE and HW acknowledge the support by the
Office of Naval Research, through grant N62909-18-1-2038, and by the DFG Collaborative
Research Center TRR 109, “Discretization in Geometry and Dynamics”, through grant
I02979-N35 of the Austrian Science Fund (FWF). PP acknowledges the support and use
of resources at the NERSC computing center.'
article_number: A163
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Pratyush
full_name: Pranav, Pratyush
last_name: Pranav
- first_name: Robert J.
full_name: Adler, Robert J.
last_name: Adler
- first_name: Thomas
full_name: Buchert, Thomas
last_name: Buchert
- first_name: Herbert
full_name: Edelsbrunner, Herbert
id: 3FB178DA-F248-11E8-B48F-1D18A9856A87
last_name: Edelsbrunner
orcid: 0000-0002-9823-6833
- first_name: Bernard J.T.
full_name: Jones, Bernard J.T.
last_name: Jones
- first_name: Armin
full_name: Schwartzman, Armin
last_name: Schwartzman
- first_name: Hubert
full_name: Wagner, Hubert
id: 379CA8B8-F248-11E8-B48F-1D18A9856A87
last_name: Wagner
- first_name: Rien
full_name: Van De Weygaert, Rien
last_name: Van De Weygaert
citation:
ama: Pranav P, Adler RJ, Buchert T, et al. Unexpected topology of the temperature
fluctuations in the cosmic microwave background. Astronomy and Astrophysics.
2019;627. doi:10.1051/0004-6361/201834916
apa: Pranav, P., Adler, R. J., Buchert, T., Edelsbrunner, H., Jones, B. J. T., Schwartzman,
A., … Van De Weygaert, R. (2019). Unexpected topology of the temperature fluctuations
in the cosmic microwave background. Astronomy and Astrophysics. EDP Sciences.
https://doi.org/10.1051/0004-6361/201834916
chicago: Pranav, Pratyush, Robert J. Adler, Thomas Buchert, Herbert Edelsbrunner,
Bernard J.T. Jones, Armin Schwartzman, Hubert Wagner, and Rien Van De Weygaert.
“Unexpected Topology of the Temperature Fluctuations in the Cosmic Microwave Background.”
Astronomy and Astrophysics. EDP Sciences, 2019. https://doi.org/10.1051/0004-6361/201834916.
ieee: P. Pranav et al., “Unexpected topology of the temperature fluctuations
in the cosmic microwave background,” Astronomy and Astrophysics, vol. 627.
EDP Sciences, 2019.
ista: Pranav P, Adler RJ, Buchert T, Edelsbrunner H, Jones BJT, Schwartzman A, Wagner
H, Van De Weygaert R. 2019. Unexpected topology of the temperature fluctuations
in the cosmic microwave background. Astronomy and Astrophysics. 627, A163.
mla: Pranav, Pratyush, et al. “Unexpected Topology of the Temperature Fluctuations
in the Cosmic Microwave Background.” Astronomy and Astrophysics, vol. 627,
A163, EDP Sciences, 2019, doi:10.1051/0004-6361/201834916.
short: P. Pranav, R.J. Adler, T. Buchert, H. Edelsbrunner, B.J.T. Jones, A. Schwartzman,
H. Wagner, R. Van De Weygaert, Astronomy and Astrophysics 627 (2019).
date_created: 2019-08-04T21:59:18Z
date_published: 2019-07-17T00:00:00Z
date_updated: 2025-05-20T08:01:55Z
day: '17'
ddc:
- '520'
- '530'
department:
- _id: HeEd
doi: 10.1051/0004-6361/201834916
external_id:
arxiv:
- '1812.07678'
isi:
- '000475839300003'
file:
- access_level: open_access
checksum: 83b9209ed9eefbdcefd89019c5a97805
content_type: application/pdf
creator: dernst
date_created: 2019-08-05T08:08:59Z
date_updated: 2020-07-14T12:47:39Z
file_id: '6766'
file_name: 2019_AstronomyAstrophysics_Pranav.pdf
file_size: 14420451
relation: main_file
file_date_updated: 2020-07-14T12:47:39Z
has_accepted_license: '1'
intvolume: ' 627'
isi: 1
language:
- iso: eng
month: '07'
oa: 1
oa_version: Published Version
project:
- _id: 265683E4-B435-11E9-9278-68D0E5697425
grant_number: M62909-18-1-2038
name: Toward Computational Information Topology
- _id: 2561EBF4-B435-11E9-9278-68D0E5697425
call_identifier: FWF
grant_number: I02979-N35
name: Persistence and stability of geometric complexes
publication: Astronomy and Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: Unexpected topology of the temperature fluctuations in the cosmic microwave
background
tmp:
image: /images/cc_by.png
legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode
name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)
short: CC BY (4.0)
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 627
year: '2019'
...
---
_id: '11508'
abstract:
- lang: eng
text: Distant luminous Lyman-α emitters (LAEs) are excellent targets for spectroscopic
observations of galaxies in the epoch of reionisation (EoR). We present deep high-resolution
(R = 5000) VLT/X-shooter observations, along with an extensive collection of photometric
data of COLA1, a proposed double peaked LAE at z = 6.6. We rule out the possibility
that COLA1’s emission line is an [OII] doublet at z = 1.475 on the basis of i)
the asymmetric red line-profile and flux ratio of the peaks (blue/red=0.31 ± 0.03)
and ii) an unphysical [OII]/Hα ratio ([OII]/Hα > 22). We show that COLA1’s observed
B-band flux is explained by a faint extended foreground LAE, for which we detect
Lyα and [OIII] at z = 2.142. We thus conclude that COLA1 is a real double-peaked
LAE at z = 6.593, the first discovered at z > 6. COLA1 is UV luminous (M1500 = −21.6 ± 0.3),
has a high equivalent width (EW0,Lyα = 120−40+50 Å) and very compact Lyα emission
(r50,Lyα = 0.33−0.04+0.07 kpc). Relatively weak inferred Hβ+[OIII] line-emission
from Spitzer/IRAC indicates an extremely low metallicity of Z < 1/20 Z⊙ or reduced
strength of nebular lines due to high escape of ionising photons. The small Lyα
peak separation of 220 ± 20 km s−1 implies a low HI column density and an ionising
photon escape fraction of ≈15 − 30%, providing the first direct evidence that
such galaxies contribute actively to the reionisation of the Universe at z > 6.
Based on simple estimates, we find that COLA1 could have provided just enough
photons to reionise its own ≈0.3 pMpc (2.3 cMpc) bubble, allowing the blue Lyα
line to be observed. However, we also discuss alternative scenarios explaining
the detected double peaked nature of COLA1. Our results show that future high-resolution
observations of statistical samples of double peaked LAEs at z > 5 are a promising
probe of the occurrence of ionised regions around galaxies in the EoR.
acknowledgement: JM acknowledges the award of a Huygens PhD fellowship from Leiden
University. MG acknowledges support from NASA grant NNX17AK58G. APA, PhD::SPACE
fellow, acknowledges support from the FCT through the fellowship PD/BD/52706/2014.
Based on observations made with ESO Telescopes at the La Silla Paranal Observatory
under programme IDs 294.A-5018, 098.A-0819, 099.A-0254 and 0100.A-0213. We are grateful
for the excellent data-sets from the COSMOS and UltraVISTA survey teams. This research
was supported by the Munich Institute for Astro- and Particle Physics (MIAPP) of
the DFG cluster of excellence “Origin and Structure of the Universe”. We thank the
referee for their comments that improved the paper. We also thank Christoph Behrens,
Len Cowie, Koki Kakiichi, Peter Laursen, Charlotte Mason, Eros Vanzella, Lewis Weinberger
and Johannes Zabl for discussions. We have benefited from the public available programming
language Python, including the numpy, matplotlib, scipy and astropy packages (Hunter
2007; Astropy Collaboration 2013), the astronomical imaging tools Swarp (Bertin
2010) and ds9 and the Topcat analysis tool (Taylor 2013).
article_number: A136
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: Max
full_name: Gronke, Max
last_name: Gronke
- first_name: Ana
full_name: Paulino-Afonso, Ana
last_name: Paulino-Afonso
- first_name: Mauro
full_name: Stefanon, Mauro
last_name: Stefanon
- first_name: Huub
full_name: Röttgering, Huub
last_name: Röttgering
citation:
ama: 'Matthee JJ, Sobral D, Gronke M, Paulino-Afonso A, Stefanon M, Röttgering H.
Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy directly
contributing to the reionisation of the universe. Astronomy & Astrophysics.
2018;619. doi:10.1051/0004-6361/201833528'
apa: 'Matthee, J. J., Sobral, D., Gronke, M., Paulino-Afonso, A., Stefanon, M.,
& Röttgering, H. (2018). Confirmation of double peaked Lyα emission at z =
6.593: Witnessing a galaxy directly contributing to the reionisation of the universe.
Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201833528'
chicago: 'Matthee, Jorryt J, David Sobral, Max Gronke, Ana Paulino-Afonso, Mauro
Stefanon, and Huub Röttgering. “Confirmation of Double Peaked Lyα Emission at
z = 6.593: Witnessing a Galaxy Directly Contributing to the Reionisation of the
Universe.” Astronomy & Astrophysics. EDP Sciences, 2018. https://doi.org/10.1051/0004-6361/201833528.'
ieee: 'J. J. Matthee, D. Sobral, M. Gronke, A. Paulino-Afonso, M. Stefanon, and
H. Röttgering, “Confirmation of double peaked Lyα emission at z = 6.593: Witnessing
a galaxy directly contributing to the reionisation of the universe,” Astronomy
& Astrophysics, vol. 619. EDP Sciences, 2018.'
ista: 'Matthee JJ, Sobral D, Gronke M, Paulino-Afonso A, Stefanon M, Röttgering
H. 2018. Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a
galaxy directly contributing to the reionisation of the universe. Astronomy &
Astrophysics. 619, A136.'
mla: 'Matthee, Jorryt J., et al. “Confirmation of Double Peaked Lyα Emission at
z = 6.593: Witnessing a Galaxy Directly Contributing to the Reionisation of the
Universe.” Astronomy & Astrophysics, vol. 619, A136, EDP Sciences,
2018, doi:10.1051/0004-6361/201833528.'
short: J.J. Matthee, D. Sobral, M. Gronke, A. Paulino-Afonso, M. Stefanon, H. Röttgering,
Astronomy & Astrophysics 619 (2018).
date_created: 2022-07-06T11:14:23Z
date_published: 2018-11-19T00:00:00Z
date_updated: 2024-10-14T11:31:36Z
day: '19'
doi: 10.1051/0004-6361/201833528
extern: '1'
external_id:
arxiv:
- '1805.11621'
intvolume: ' 619'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: high-redshift / galaxies: formation / dark ages / reionization / first
stars / techniques: spectroscopic / intergalactic medium'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1805.11621
month: '11'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Confirmation of double peaked Lyα emission at z = 6.593: Witnessing a galaxy
directly contributing to the reionisation of the universe'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 619
year: '2018'
...
---
_id: '11618'
abstract:
- lang: eng
text: Asteroseismology provides global stellar parameters such as masses, radii,
or surface gravities using mean global seismic parameters and effective temperature
for thousands of low-mass stars (0.8 M⊙ < M < 3 M⊙). This methodology has been
successfully applied to stars in which acoustic modes excited by turbulent convection
are measured. Other methods such as the Flicker technique can also be used to
determine stellar surface gravities, but only works for log g above 2.5 dex. In
this work, we present a new metric called FliPer (Flicker in spectral power density,
in opposition to the standard Flicker measurement which is computed in the time
domain); it is able to extend the range for which reliable surface gravities can
be obtained (0.1 < log g < 4.6 dex) without performing any seismic analysis for
stars brighter than Kp < 14. FliPer takes into account the average variability
of a star measured in the power density spectrum in a given range of frequencies.
However, FliPer values calculated on several ranges of frequency are required
to better characterize a star. Using a large set of asteroseismic targets it is
possible to calibrate the behavior of surface gravity with FliPer through machine
learning. This calibration made with a random forest regressor covers a wide range
of surface gravities from main-sequence stars to subgiants and red giants, with
very small uncertainties from 0.04 to 0.1 dex. FliPer values can be inserted in
automatic global seismic pipelines to either give an estimation of the stellar
surface gravity or to assess the quality of the seismic results by detecting any
outliers in the obtained νmax values. FliPer also constrains the surface gravities
of main-sequence dwarfs using only long-cadence data for which the Nyquist frequency
is too low to measure the acoustic-mode properties.
acknowledgement: We thank the anonymous referee for the very useful comments. We would
also like to thank M. Benbakoura for his help in analyzing the light curves of several
binary systems included in our set of stars. L.B. and R.A.G. acknowledge the support
from PLATO and GOLF CNES grants. S.M. acknowledges support from the National Aeronautics
and Space Administration under Grant NNX15AF13G, the National Science Foundation
grant AST-1411685, and the Ramon y Cajal fellowship no. RYC-2015-17697. E.C. is
funded by the European Union’s Horizon 2020 research and innovation program under
the Marie Sklodowska-Curie grant agreement no. 664931. O.J.H and B.M.R. acknowledge
the support of the UK Science and Technology Facilities Council (STFC). Funding
for the Stellar Astrophysics Centre is provided by the Danish National Research
Foundation (Grant DNRF106). This research has made use of NASA’s Astrophysics Data
System. Data presented in this paper were obtained from the Mikulski Archive for
Space Telescopes (MAST). STScI is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS5-26555.
article_number: A38
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Lisa Annabelle
full_name: Bugnet, Lisa Annabelle
id: d9edb345-f866-11ec-9b37-d119b5234501
last_name: Bugnet
orcid: 0000-0003-0142-4000
- first_name: R. A.
full_name: García, R. A.
last_name: García
- first_name: G. R.
full_name: Davies, G. R.
last_name: Davies
- first_name: S.
full_name: Mathur, S.
last_name: Mathur
- first_name: E.
full_name: Corsaro, E.
last_name: Corsaro
- first_name: O. J.
full_name: Hall, O. J.
last_name: Hall
- first_name: B. M.
full_name: Rendle, B. M.
last_name: Rendle
citation:
ama: 'Bugnet LA, García RA, Davies GR, et al. FliPer: A global measure of power
density to estimate surface gravities of main-sequence solar-like stars and red
giants. Astronomy & Astrophysics. 2018;620. doi:10.1051/0004-6361/201833106'
apa: 'Bugnet, L. A., García, R. A., Davies, G. R., Mathur, S., Corsaro, E., Hall,
O. J., & Rendle, B. M. (2018). FliPer: A global measure of power density to
estimate surface gravities of main-sequence solar-like stars and red giants. Astronomy
& Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201833106'
chicago: 'Bugnet, Lisa Annabelle, R. A. García, G. R. Davies, S. Mathur, E. Corsaro,
O. J. Hall, and B. M. Rendle. “FliPer: A Global Measure of Power Density to Estimate
Surface Gravities of Main-Sequence Solar-like Stars and Red Giants.” Astronomy
& Astrophysics. EDP Sciences, 2018. https://doi.org/10.1051/0004-6361/201833106.'
ieee: 'L. A. Bugnet et al., “FliPer: A global measure of power density to
estimate surface gravities of main-sequence solar-like stars and red giants,”
Astronomy & Astrophysics, vol. 620. EDP Sciences, 2018.'
ista: 'Bugnet LA, García RA, Davies GR, Mathur S, Corsaro E, Hall OJ, Rendle BM.
2018. FliPer: A global measure of power density to estimate surface gravities
of main-sequence solar-like stars and red giants. Astronomy & Astrophysics.
620, A38.'
mla: 'Bugnet, Lisa Annabelle, et al. “FliPer: A Global Measure of Power Density
to Estimate Surface Gravities of Main-Sequence Solar-like Stars and Red Giants.”
Astronomy & Astrophysics, vol. 620, A38, EDP Sciences, 2018, doi:10.1051/0004-6361/201833106.'
short: L.A. Bugnet, R.A. García, G.R. Davies, S. Mathur, E. Corsaro, O.J. Hall,
B.M. Rendle, Astronomy & Astrophysics 620 (2018).
date_created: 2022-07-18T14:37:39Z
date_published: 2018-12-01T00:00:00Z
date_updated: 2024-10-14T11:40:17Z
day: '01'
doi: 10.1051/0004-6361/201833106
extern: '1'
external_id:
arxiv:
- '1809.05105'
intvolume: ' 620'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- asteroseismology / methods
- data analysis / stars
- oscillations
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1809.05105
month: '12'
oa: 1
oa_version: Preprint
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'FliPer: A global measure of power density to estimate surface gravities of
main-sequence solar-like stars and red giants'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 620
year: '2018'
...
---
_id: '11619'
abstract:
- lang: eng
text: We report on the confirmation and mass determination of π Men c, the first
transiting planet discovered by NASA’s TESS space mission. π Men is a naked-eye
(V = 5.65 mag), quiet G0 V star that was previously known to host a sub-stellar
companion (π Men b) on a longperiod (Porb = 2091 days), eccentric (e = 0.64) orbit.
Using TESS time-series photometry, combined with Gaia data, published UCLES at
AAT Doppler measurements, and archival HARPS at ESO-3.6m radial velocities, we
found that π Men c is a close-in planet with an orbital period of Porb = 6.27
days, a mass of Mc = 4.52 ± 0.81 M⊕, and a radius of Rc = 2.06 ± 0.03 R⊕. Based
on the planet’s orbital period and size, π Men c is a super-Earth located at,
or close to, the radius gap, while its mass and bulk density suggest it may have
held on to a significant atmosphere. Because of the brightness of the host star,
this system is highly suitable for a wide range of further studies to characterize
the planetary atmosphere and dynamical properties. We also performed an asteroseismic
analysis of the TESS data and detected a hint of power excess consistent with
the seismic values expected for this star, although this result depends on the
photometric aperture used to extract the light curve. This marginal detection
is expected from pre-launch simulations hinting at the asteroseismic potential
of the TESS mission for longer, multi-sector observations and/or for more evolved
bright stars.
article_number: L10
article_processing_charge: No
article_type: letter_note
arxiv: 1
author:
- first_name: D.
full_name: Gandolfi, D.
last_name: Gandolfi
- first_name: O.
full_name: Barragán, O.
last_name: Barragán
- first_name: J. H.
full_name: Livingston, J. H.
last_name: Livingston
- first_name: M.
full_name: Fridlund, M.
last_name: Fridlund
- first_name: A. B.
full_name: Justesen, A. B.
last_name: Justesen
- first_name: S.
full_name: Redfield, S.
last_name: Redfield
- first_name: L.
full_name: Fossati, L.
last_name: Fossati
- first_name: S.
full_name: Mathur, S.
last_name: Mathur
- first_name: S.
full_name: Grziwa, S.
last_name: Grziwa
- first_name: J.
full_name: Cabrera, J.
last_name: Cabrera
- first_name: R. A.
full_name: García, R. A.
last_name: García
- first_name: C. M.
full_name: Persson, C. M.
last_name: Persson
- first_name: V.
full_name: Van Eylen, V.
last_name: Van Eylen
- first_name: A. P.
full_name: Hatzes, A. P.
last_name: Hatzes
- first_name: D.
full_name: Hidalgo, D.
last_name: Hidalgo
- first_name: S.
full_name: Albrecht, S.
last_name: Albrecht
- first_name: Lisa Annabelle
full_name: Bugnet, Lisa Annabelle
id: d9edb345-f866-11ec-9b37-d119b5234501
last_name: Bugnet
orcid: 0000-0003-0142-4000
- first_name: W. D.
full_name: Cochran, W. D.
last_name: Cochran
- first_name: Sz.
full_name: Csizmadia, Sz.
last_name: Csizmadia
- first_name: H.
full_name: Deeg, H.
last_name: Deeg
- first_name: Ph.
full_name: Eigmüller, Ph.
last_name: Eigmüller
- first_name: M.
full_name: Endl, M.
last_name: Endl
- first_name: A.
full_name: Erikson, A.
last_name: Erikson
- first_name: M.
full_name: Esposito, M.
last_name: Esposito
- first_name: E.
full_name: Guenther, E.
last_name: Guenther
- first_name: J.
full_name: Korth, J.
last_name: Korth
- first_name: R.
full_name: Luque, R.
last_name: Luque
- first_name: P.
full_name: Montañes Rodríguez, P.
last_name: Montañes Rodríguez
- first_name: D.
full_name: Nespral, D.
last_name: Nespral
- first_name: G.
full_name: Nowak, G.
last_name: Nowak
- first_name: M.
full_name: Pätzold, M.
last_name: Pätzold
- first_name: J.
full_name: Prieto-Arranz, J.
last_name: Prieto-Arranz
citation:
ama: 'Gandolfi D, Barragán O, Livingston JH, et al. TESS’s first planet: A super-Earth
transiting the naked-eye star π Mensae. Astronomy & Astrophysics. 2018;619.
doi:10.1051/0004-6361/201834289'
apa: 'Gandolfi, D., Barragán, O., Livingston, J. H., Fridlund, M., Justesen, A.
B., Redfield, S., … Prieto-Arranz, J. (2018). TESS’s first planet: A super-Earth
transiting the naked-eye star π Mensae. Astronomy & Astrophysics. EDP
Sciences. https://doi.org/10.1051/0004-6361/201834289'
chicago: 'Gandolfi, D., O. Barragán, J. H. Livingston, M. Fridlund, A. B. Justesen,
S. Redfield, L. Fossati, et al. “TESS’s First Planet: A Super-Earth Transiting
the Naked-Eye Star π Mensae.” Astronomy & Astrophysics. EDP Sciences,
2018. https://doi.org/10.1051/0004-6361/201834289.'
ieee: 'D. Gandolfi et al., “TESS’s first planet: A super-Earth transiting
the naked-eye star π Mensae,” Astronomy & Astrophysics, vol. 619. EDP
Sciences, 2018.'
ista: 'Gandolfi D, Barragán O, Livingston JH, Fridlund M, Justesen AB, Redfield
S, Fossati L, Mathur S, Grziwa S, Cabrera J, García RA, Persson CM, Van Eylen
V, Hatzes AP, Hidalgo D, Albrecht S, Bugnet LA, Cochran WD, Csizmadia S, Deeg
H, Eigmüller P, Endl M, Erikson A, Esposito M, Guenther E, Korth J, Luque R, Montañes
Rodríguez P, Nespral D, Nowak G, Pätzold M, Prieto-Arranz J. 2018. TESS’s first
planet: A super-Earth transiting the naked-eye star π Mensae. Astronomy &
Astrophysics. 619, L10.'
mla: 'Gandolfi, D., et al. “TESS’s First Planet: A Super-Earth Transiting the Naked-Eye
Star π Mensae.” Astronomy & Astrophysics, vol. 619, L10, EDP Sciences,
2018, doi:10.1051/0004-6361/201834289.'
short: D. Gandolfi, O. Barragán, J.H. Livingston, M. Fridlund, A.B. Justesen, S.
Redfield, L. Fossati, S. Mathur, S. Grziwa, J. Cabrera, R.A. García, C.M. Persson,
V. Van Eylen, A.P. Hatzes, D. Hidalgo, S. Albrecht, L.A. Bugnet, W.D. Cochran,
S. Csizmadia, H. Deeg, P. Eigmüller, M. Endl, A. Erikson, M. Esposito, E. Guenther,
J. Korth, R. Luque, P. Montañes Rodríguez, D. Nespral, G. Nowak, M. Pätzold, J.
Prieto-Arranz, Astronomy & Astrophysics 619 (2018).
date_created: 2022-07-18T14:41:16Z
date_published: 2018-11-22T00:00:00Z
date_updated: 2022-08-22T07:43:29Z
day: '22'
doi: 10.1051/0004-6361/201834289
extern: '1'
external_id:
arxiv:
- '1809.07573'
intvolume: ' 619'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- planetary systems / planets and satellites
- detection / planets and satellites
- fundamental parameters / planets and satellites
- terrestrial planets / stars
- fundamental parameters
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1809.07573
month: '11'
oa: 1
oa_version: Preprint
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'TESS’s first planet: A super-Earth transiting the naked-eye star π Mensae'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 619
year: '2018'
...
---
_id: '13473'
abstract:
- lang: eng
text: Stripped-envelope stars form in binary systems after losing mass through Roche-lobe
overflow. They bear astrophysical significance as sources of UV and ionizing radiation
in older stellar populations and, if sufficiently massive, as stripped supernova
progenitors. Binary evolutionary models predict that they are common, but only
a handful of subdwarfs with B-type companions are known. The question is whether
a large population of such systems has evaded detection as a result of biases,
or whether the model predictions are wrong. We reanalyze the well-studied post-interaction
binary φ Persei. Recently, new data have improved the orbital solution of the
system, which contains an ~1.2M⊙ stripped-envelope star and a rapidly rotating
~9.6M⊙ Be star. We compare with an extensive grid of evolutionary models using
a Bayesian approach and constrain the initial masses of the progenitor to 7.2
± 0.4M⊙ for the stripped star and 3.8 ± 0.4M⊙ for the Be star. The system must
have evolved through near-conservative mass transfer. These findings are consistent
with earlier studies. The age we obtain, 57 ± 9 Myr, is in excellent agreement
with the age of the α Persei cluster. We note that neither star was initially
massive enough to produce a core-collapse supernova, but mass exchange pushed
the Be star above the mass threshold. We find that the subdwarf is overluminous
for its mass by almost an order of magnitude, compared to the expectations for
a helium core burning star. We can only reconcile this if the subdwarf resides
in a late phase of helium shell burning, which lasts only 2–3% of the total lifetime
as a subdwarf. Assuming continuous star formation implies that up to ~50 less
evolved, dimmer subdwarfs exist for each system similar to φ Persei, but have
evaded detection so far. Our findings can be interpreted as a strong indication
that a substantial population of stripped-envelope stars indeed exists, but has
so far evaded detection because of observational biases and lack of large-scale
systematic searches.
article_number: A30
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: A.
full_name: Schootemeijer, A.
last_name: Schootemeijer
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: S. E.
full_name: de Mink, S. E.
last_name: de Mink
- first_name: D.
full_name: Gies, D.
last_name: Gies
- first_name: E.
full_name: Zapartas, E.
last_name: Zapartas
citation:
ama: Schootemeijer A, Götberg YLL, de Mink SE, Gies D, Zapartas E. Clues about the
scarcity of stripped-envelope stars from the evolutionary state of the sdO+Be
binary system φ Persei. Astronomy & Astrophysics. 2018;615. doi:10.1051/0004-6361/201731194
apa: Schootemeijer, A., Götberg, Y. L. L., de Mink, S. E., Gies, D., & Zapartas,
E. (2018). Clues about the scarcity of stripped-envelope stars from the evolutionary
state of the sdO+Be binary system φ Persei. Astronomy & Astrophysics.
EDP Sciences. https://doi.org/10.1051/0004-6361/201731194
chicago: Schootemeijer, A., Ylva Louise Linsdotter Götberg, S. E. de Mink, D. Gies,
and E. Zapartas. “Clues about the Scarcity of Stripped-Envelope Stars from the
Evolutionary State of the SdO+Be Binary System φ Persei.” Astronomy & Astrophysics.
EDP Sciences, 2018. https://doi.org/10.1051/0004-6361/201731194.
ieee: A. Schootemeijer, Y. L. L. Götberg, S. E. de Mink, D. Gies, and E. Zapartas,
“Clues about the scarcity of stripped-envelope stars from the evolutionary state
of the sdO+Be binary system φ Persei,” Astronomy & Astrophysics, vol.
615. EDP Sciences, 2018.
ista: Schootemeijer A, Götberg YLL, de Mink SE, Gies D, Zapartas E. 2018. Clues
about the scarcity of stripped-envelope stars from the evolutionary state of the
sdO+Be binary system φ Persei. Astronomy & Astrophysics. 615, A30.
mla: Schootemeijer, A., et al. “Clues about the Scarcity of Stripped-Envelope Stars
from the Evolutionary State of the SdO+Be Binary System φ Persei.” Astronomy
& Astrophysics, vol. 615, A30, EDP Sciences, 2018, doi:10.1051/0004-6361/201731194.
short: A. Schootemeijer, Y.L.L. Götberg, S.E. de Mink, D. Gies, E. Zapartas, Astronomy
& Astrophysics 615 (2018).
date_created: 2023-08-03T10:14:37Z
date_published: 2018-07-06T00:00:00Z
date_updated: 2023-08-09T12:22:52Z
day: '06'
doi: 10.1051/0004-6361/201731194
extern: '1'
external_id:
arxiv:
- '1803.02379'
intvolume: ' 615'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1051/0004-6361/201731194
month: '07'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: Clues about the scarcity of stripped-envelope stars from the evolutionary state
of the sdO+Be binary system φ Persei
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 615
year: '2018'
...
---
_id: '13475'
abstract:
- lang: eng
text: Stars stripped of their hydrogen-rich envelope through interaction with a
binary companion are generally not considered when accounting for ionizing radiation
from stellar populations, despite the expectation that stripped stars emit hard
ionizing radiation, form frequently, and live 10–100 times longer than single
massive stars. We compute the first grid of evolutionary and spectral models specially
made for stars stripped in binaries for a range of progenitor masses (2–20 M⊙)
and metallicities ranging from solar to values representative for pop II stars.
For stripped stars with masses in the range 0.3–7 M⊙, we find consistently high
effective temperatures (20 000–100 000 K, increasing with mass), small radii (0.2–1
R⊙), and high bolometric luminosities, comparable to that of their progenitor
before stripping. The spectra show a continuous sequence that naturally bridges
subdwarf-type stars at the low-mass end and Wolf-Rayet-like spectra at the high-mass
end. For intermediate masses we find hybrid spectral classes showing a mixture
of absorption and emission lines. These appear for stars with mass-loss rates
of 10−8−10−6 M⊙ yr−1, which have semi-transparent atmospheres. At low metallicity,
substantial hydrogen-rich layers are left at the surface and we predict spectra
that resemble O-type stars instead. We obtain spectra undistinguishable from subdwarfs
for stripped stars with masses up to 1.7 M⊙, which questions whether the widely
adopted canonical value of 0.47 M⊙ is uniformly valid. Only a handful of stripped
stars of intermediate mass have currently been identified observationally. Increasing
this sample will provide necessary tests for the physics of interaction, internal
mixing, and stellar winds. We use our model spectra to investigate the feasibility
to detect stripped stars next to an optically bright companion and recommend systematic
searches for their UV excess and possible emission lines, most notably HeII λ4686
in the optical and HeII λ1640 in the UV. Our models are publicly available for
further investigations or inclusion in spectral synthesis simulations.
article_number: A78
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: S. E.
full_name: de Mink, S. E.
last_name: de Mink
- first_name: J. H.
full_name: Groh, J. H.
last_name: Groh
- first_name: T.
full_name: Kupfer, T.
last_name: Kupfer
- first_name: P. A.
full_name: Crowther, P. A.
last_name: Crowther
- first_name: E.
full_name: Zapartas, E.
last_name: Zapartas
- first_name: M.
full_name: Renzo, M.
last_name: Renzo
citation:
ama: 'Götberg YLL, de Mink SE, Groh JH, et al. Spectral models for binary products:
Unifying subdwarfs and Wolf-Rayet stars as a sequence of stripped-envelope stars.
Astronomy & Astrophysics. 2018;615. doi:10.1051/0004-6361/201732274'
apa: 'Götberg, Y. L. L., de Mink, S. E., Groh, J. H., Kupfer, T., Crowther, P. A.,
Zapartas, E., & Renzo, M. (2018). Spectral models for binary products: Unifying
subdwarfs and Wolf-Rayet stars as a sequence of stripped-envelope stars. Astronomy
& Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201732274'
chicago: 'Götberg, Ylva Louise Linsdotter, S. E. de Mink, J. H. Groh, T. Kupfer,
P. A. Crowther, E. Zapartas, and M. Renzo. “Spectral Models for Binary Products:
Unifying Subdwarfs and Wolf-Rayet Stars as a Sequence of Stripped-Envelope Stars.”
Astronomy & Astrophysics. EDP Sciences, 2018. https://doi.org/10.1051/0004-6361/201732274.'
ieee: 'Y. L. L. Götberg et al., “Spectral models for binary products: Unifying
subdwarfs and Wolf-Rayet stars as a sequence of stripped-envelope stars,” Astronomy
& Astrophysics, vol. 615. EDP Sciences, 2018.'
ista: 'Götberg YLL, de Mink SE, Groh JH, Kupfer T, Crowther PA, Zapartas E, Renzo
M. 2018. Spectral models for binary products: Unifying subdwarfs and Wolf-Rayet
stars as a sequence of stripped-envelope stars. Astronomy & Astrophysics.
615, A78.'
mla: 'Götberg, Ylva Louise Linsdotter, et al. “Spectral Models for Binary Products:
Unifying Subdwarfs and Wolf-Rayet Stars as a Sequence of Stripped-Envelope Stars.”
Astronomy & Astrophysics, vol. 615, A78, EDP Sciences, 2018, doi:10.1051/0004-6361/201732274.'
short: Y.L.L. Götberg, S.E. de Mink, J.H. Groh, T. Kupfer, P.A. Crowther, E. Zapartas,
M. Renzo, Astronomy & Astrophysics 615 (2018).
date_created: 2023-08-03T10:15:00Z
date_published: 2018-07-17T00:00:00Z
date_updated: 2024-10-14T12:22:18Z
day: '17'
doi: 10.1051/0004-6361/201732274
extern: '1'
external_id:
arxiv:
- '1802.03018'
intvolume: ' 615'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1051/0004-6361/201732274
month: '07'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Spectral models for binary products: Unifying subdwarfs and Wolf-Rayet stars
as a sequence of stripped-envelope stars'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 615
year: '2018'
...
---
_id: '13476'
abstract:
- lang: eng
text: Understanding ionizing fluxes of stellar populations is crucial for various
astrophysical problems including the epoch of reionization. Short-lived massive
stars are generally considered as the main stellar sources. We examine the potential
role of less massive stars that lose their envelope through interaction with a
binary companion. Here, we focus on the role of metallicity (Z). For this purpose
we used the evolutionary code MESA and created tailored atmosphere models with
the radiative transfer code CMFGEN. We show that typical progenitors, with initial
masses of 12 M⊙, produce hot and compact stars (~ 4 M⊙, 60–80 kK, ~1 R⊙). These
stripped stars copiously produce ionizing photons, emitting 60–85% and 30–60%
of their energy as HI and HeI ionizing radiation, for Z = 0.0001–0.02, respectively.
Their output is comparable to what massive stars emit during their Wolf-Rayet
phase, if we account for their longer lifetimes and the favorable slope of the
initial mass function. Their relative importance for reionization may be further
favored since they emit their photons with a time delay (~ 20 Myr after birth
in our fiducial model). This allows time for the dispersal of the birth clouds,
allowing the ionizing photons to escape into the intergalactic medium. At low
Z, we find that Roche stripping fails to fully remove the H-rich envelope, because
of the reduced opacity in the subsurface layers. This is in sharp contrast with
the assumption of complete stripping that is made in rapid population synthesis
simulations, which are widely used to simulate the binary progenitors of supernovae
and gravitational waves. Finally, we discuss the urgency to increase the observed
sample of stripped stars to test these models and we discuss how our predictions
can help to design efficient observational campaigns.
article_number: A11
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: S. E.
full_name: de Mink, S. E.
last_name: de Mink
- first_name: J. H.
full_name: Groh, J. H.
last_name: Groh
citation:
ama: 'Götberg YLL, de Mink SE, Groh JH. Ionizing spectra of stars that lose their
envelope through interaction with a binary companion: Role of metallicity. Astronomy
& Astrophysics. 2017;608. doi:10.1051/0004-6361/201730472'
apa: 'Götberg, Y. L. L., de Mink, S. E., & Groh, J. H. (2017). Ionizing spectra
of stars that lose their envelope through interaction with a binary companion:
Role of metallicity. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201730472'
chicago: 'Götberg, Ylva Louise Linsdotter, S. E. de Mink, and J. H. Groh. “Ionizing
Spectra of Stars That Lose Their Envelope through Interaction with a Binary Companion:
Role of Metallicity.” Astronomy & Astrophysics. EDP Sciences, 2017.
https://doi.org/10.1051/0004-6361/201730472.'
ieee: 'Y. L. L. Götberg, S. E. de Mink, and J. H. Groh, “Ionizing spectra of stars
that lose their envelope through interaction with a binary companion: Role of
metallicity,” Astronomy & Astrophysics, vol. 608. EDP Sciences, 2017.'
ista: 'Götberg YLL, de Mink SE, Groh JH. 2017. Ionizing spectra of stars that lose
their envelope through interaction with a binary companion: Role of metallicity.
Astronomy & Astrophysics. 608, A11.'
mla: 'Götberg, Ylva Louise Linsdotter, et al. “Ionizing Spectra of Stars That Lose
Their Envelope through Interaction with a Binary Companion: Role of Metallicity.”
Astronomy & Astrophysics, vol. 608, A11, EDP Sciences, 2017, doi:10.1051/0004-6361/201730472.'
short: Y.L.L. Götberg, S.E. de Mink, J.H. Groh, Astronomy & Astrophysics 608
(2017).
date_created: 2023-08-03T10:15:09Z
date_published: 2017-12-01T00:00:00Z
date_updated: 2024-10-14T12:22:29Z
day: '01'
doi: 10.1051/0004-6361/201730472
extern: '1'
external_id:
arxiv:
- '1701.07439'
intvolume: ' 608'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1051/0004-6361/201730472
month: '12'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Ionizing spectra of stars that lose their envelope through interaction with
a binary companion: Role of metallicity'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 608
year: '2017'
...
---
_id: '13477'
abstract:
- lang: eng
text: Most massive stars, the progenitors of core-collapse supernovae, are in close
binary systems and may interact with their companion through mass transfer or
merging. We undertake a population synthesis study to compute the delay-time distribution
of core-collapse supernovae, that is, the supernova rate versus time following
a starburst, taking into account binary interactions. We test the systematic robustness
of our results by running various simulations to account for the uncertainties
in our standard assumptions. We find that a significant fraction, 15+9-8%, of
core-collapse supernovae are “late”, that is, they occur 50–200 Myr after birth,
when all massive single stars have already exploded. These late events originate
predominantly from binary systems with at least one, or, in most cases, with both
stars initially being of intermediate mass (4–8 M⊙). The main evolutionary channels
that contribute often involve either the merging of the initially more massive
primary star with its companion or the engulfment of the remaining core of the
primary by the expanding secondary that has accreted mass at an earlier evolutionary
stage. Also, the total number of core-collapse supernovae increases by 14+15-14%
because of binarity for the same initial stellar mass. The high rate implies that
we should have already observed such late core-collapse supernovae, but have not
recognized them as such. We argue that φ Persei is a likely progenitor and that
eccentric neutron star – white dwarf systems are likely descendants. Late events
can help explain the discrepancy in the delay-time distributions derived from
supernova remnants in the Magellanic Clouds and extragalactic type Ia events,
lowering the contribution of prompt Ia events. We discuss ways to test these predictions
and speculate on the implications for supernova feedback in simulations of galaxy
evolution.
article_number: A29
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: E.
full_name: Zapartas, E.
last_name: Zapartas
- first_name: S. E.
full_name: de Mink, S. E.
last_name: de Mink
- first_name: R. G.
full_name: Izzard, R. G.
last_name: Izzard
- first_name: S.-C.
full_name: Yoon, S.-C.
last_name: Yoon
- first_name: C.
full_name: Badenes, C.
last_name: Badenes
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: A.
full_name: de Koter, A.
last_name: de Koter
- first_name: C. J.
full_name: Neijssel, C. J.
last_name: Neijssel
- first_name: M.
full_name: Renzo, M.
last_name: Renzo
- first_name: A.
full_name: Schootemeijer, A.
last_name: Schootemeijer
- first_name: T. S.
full_name: Shrotriya, T. S.
last_name: Shrotriya
citation:
ama: Zapartas E, de Mink SE, Izzard RG, et al. Delay-time distribution of core-collapse
supernovae with late events resulting from binary interaction. Astronomy &
Astrophysics. 2017;601(A&A). doi:10.1051/0004-6361/201629685
apa: Zapartas, E., de Mink, S. E., Izzard, R. G., Yoon, S.-C., Badenes, C., Götberg,
Y. L. L., … Shrotriya, T. S. (2017). Delay-time distribution of core-collapse
supernovae with late events resulting from binary interaction. Astronomy &
Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201629685
chicago: Zapartas, E., S. E. de Mink, R. G. Izzard, S.-C. Yoon, C. Badenes, Ylva
Louise Linsdotter Götberg, A. de Koter, et al. “Delay-Time Distribution of Core-Collapse
Supernovae with Late Events Resulting from Binary Interaction.” Astronomy &
Astrophysics. EDP Sciences, 2017. https://doi.org/10.1051/0004-6361/201629685.
ieee: E. Zapartas et al., “Delay-time distribution of core-collapse supernovae
with late events resulting from binary interaction,” Astronomy & Astrophysics,
vol. 601, no. A&A. EDP Sciences, 2017.
ista: Zapartas E, de Mink SE, Izzard RG, Yoon S-C, Badenes C, Götberg YLL, de Koter
A, Neijssel CJ, Renzo M, Schootemeijer A, Shrotriya TS. 2017. Delay-time distribution
of core-collapse supernovae with late events resulting from binary interaction.
Astronomy & Astrophysics. 601(A&A), A29.
mla: Zapartas, E., et al. “Delay-Time Distribution of Core-Collapse Supernovae with
Late Events Resulting from Binary Interaction.” Astronomy & Astrophysics,
vol. 601, no. A&A, A29, EDP Sciences, 2017, doi:10.1051/0004-6361/201629685.
short: E. Zapartas, S.E. de Mink, R.G. Izzard, S.-C. Yoon, C. Badenes, Y.L.L. Götberg,
A. de Koter, C.J. Neijssel, M. Renzo, A. Schootemeijer, T.S. Shrotriya, Astronomy
& Astrophysics 601 (2017).
date_created: 2023-08-03T10:15:18Z
date_published: 2017-05-01T00:00:00Z
date_updated: 2023-08-09T11:15:49Z
day: '01'
doi: 10.1051/0004-6361/201629685
extern: '1'
external_id:
arxiv:
- '1701.07032'
intvolume: ' 601'
issue: A&A
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1051/0004-6361/201629685
month: '05'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: Delay-time distribution of core-collapse supernovae with late events resulting
from binary interaction
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 601
year: '2017'
...
---
_id: '13478'
abstract:
- lang: eng
text: HR 8799 is a star accompanied by four massive planets on wide orbits. The
observed planetary configuration has been shown to be unstable on a timescale
much shorter than the estimated age of the system (~30 Myr) unless the planets
are locked into mean motion resonances. This condition is characterised by small-amplitude
libration of one or more resonant angles that stabilise the system by preventing
close encounters. We simulate planetary systems similar to the HR 8799 planetary
system, exploring the parameter space in separation between the orbits, planetary
masses and distance from the Sun to the star. We find systems that look like HR
8799 and remain stable for longer than the estimated age of HR 8799. None of our
systems are forced into resonances. We find, with nominal masses (Mb = 5 MJup
and Mc,d,e = 7 MJup) and in a narrow range of orbit separations, that 5 of 100
systems match the observations and lifetime. Considering a broad range of orbit
separations, we find 12 of 900 similar systems. The systems survive significantly
longer because of their slightly increased initial orbit separations compared
to assuming circular orbits from the observed positions. A small increase in separation
leads to a significant increase in survival time. The low eccentricity the orbits
develop from gravitational interaction is enough for the planets to match the
observations. With lower masses, but still comfortably within the estimated planet
mass uncertainty, we find 18 of 100 matching and long-lived systems in a narrow
orbital separation range. In the broad separation range, we find 82 of 900 matching
systems. Our results imply that the planets in the HR 8799 system do not have
to be in strong mean motion resonances. We also investigate the future of wide-orbit
planetary systems using our HR 8799 analogues. We find that 80% of the systems
have two planets left after strong planet-planet scattering and these are on eccentric
orbits with semi-major axes of a1 ~ 10 AU and a2 ~ 30−1000 AU. We speculate that
other wide-orbit planetary systems, such as AB Pic and HD 106906, are the remnants
of HR 8799 analogues that underwent close encounters and dynamical instability.
article_number: A147
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Ylva Louise Linsdotter
full_name: Götberg, Ylva Louise Linsdotter
id: d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d
last_name: Götberg
orcid: 0000-0002-6960-6911
- first_name: Melvyn B.
full_name: Davies, Melvyn B.
last_name: Davies
- first_name: Alexander J.
full_name: Mustill, Alexander J.
last_name: Mustill
- first_name: Anders
full_name: Johansen, Anders
last_name: Johansen
- first_name: Ross P.
full_name: Church, Ross P.
last_name: Church
citation:
ama: Götberg YLL, Davies MB, Mustill AJ, Johansen A, Church RP. Long-term stability
of the HR 8799 planetary system without resonant lock. Astronomy & Astrophysics.
2016;592. doi:10.1051/0004-6361/201526309
apa: Götberg, Y. L. L., Davies, M. B., Mustill, A. J., Johansen, A., & Church,
R. P. (2016). Long-term stability of the HR 8799 planetary system without resonant
lock. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/201526309
chicago: Götberg, Ylva Louise Linsdotter, Melvyn B. Davies, Alexander J. Mustill,
Anders Johansen, and Ross P. Church. “Long-Term Stability of the HR 8799 Planetary
System without Resonant Lock.” Astronomy & Astrophysics. EDP Sciences,
2016. https://doi.org/10.1051/0004-6361/201526309.
ieee: Y. L. L. Götberg, M. B. Davies, A. J. Mustill, A. Johansen, and R. P. Church,
“Long-term stability of the HR 8799 planetary system without resonant lock,” Astronomy
& Astrophysics, vol. 592. EDP Sciences, 2016.
ista: Götberg YLL, Davies MB, Mustill AJ, Johansen A, Church RP. 2016. Long-term
stability of the HR 8799 planetary system without resonant lock. Astronomy &
Astrophysics. 592, A147.
mla: Götberg, Ylva Louise Linsdotter, et al. “Long-Term Stability of the HR 8799
Planetary System without Resonant Lock.” Astronomy & Astrophysics,
vol. 592, A147, EDP Sciences, 2016, doi:10.1051/0004-6361/201526309.
short: Y.L.L. Götberg, M.B. Davies, A.J. Mustill, A. Johansen, R.P. Church, Astronomy
& Astrophysics 592 (2016).
date_created: 2023-08-03T10:15:28Z
date_published: 2016-08-18T00:00:00Z
date_updated: 2024-10-14T12:22:01Z
day: '18'
doi: 10.1051/0004-6361/201526309
extern: '1'
external_id:
arxiv:
- '1606.07819'
intvolume: ' 592'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1051/0004-6361/201526309
month: '08'
oa: 1
oa_version: Published Version
publication: Astronomy & Astrophysics
publication_identifier:
eissn:
- 1432-0746
issn:
- 0004-6361
publication_status: published
publisher: EDP Sciences
quality_controlled: '1'
scopus_import: '1'
status: public
title: Long-term stability of the HR 8799 planetary system without resonant lock
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 592
year: '2016'
...