{"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1111/j.1365-2966.2010.18080.x"}],"status":"public","day":"08","issue":"4","language":[{"iso":"eng"}],"article_type":"original","date_published":"2011-04-08T00:00:00Z","alternative_title":["Suppression of HD cooling in primordial gas"],"author":[{"first_name":"J.","full_name":"Wolcott-Green, J.","last_name":"Wolcott-Green"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","full_name":"Haiman, Zoltán","first_name":"Zoltán"}],"page":"2603-2616","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","date_created":"2024-09-06T07:52:22Z","oa_version":"Published Version","date_updated":"2024-09-25T08:47:23Z","citation":{"mla":"Wolcott-Green, J., and Zoltán Haiman. “Suppression of HD Cooling in Protogalactic Gas Clouds by Lyman-Werner Radiation.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 412, no. 4, Oxford University Press, 2011, pp. 2603–16, doi:<a href=\"https://doi.org/10.1111/j.1365-2966.2010.18080.x\">10.1111/j.1365-2966.2010.18080.x</a>.","chicago":"Wolcott-Green, J., and Zoltán Haiman. “Suppression of HD Cooling in Protogalactic Gas Clouds by Lyman-Werner Radiation.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2011. <a href=\"https://doi.org/10.1111/j.1365-2966.2010.18080.x\">https://doi.org/10.1111/j.1365-2966.2010.18080.x</a>.","short":"J. Wolcott-Green, Z. Haiman, Monthly Notices of the Royal Astronomical Society 412 (2011) 2603–2616.","ama":"Wolcott-Green J, Haiman Z. Suppression of HD cooling in protogalactic gas clouds by Lyman-Werner radiation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2011;412(4):2603-2616. doi:<a href=\"https://doi.org/10.1111/j.1365-2966.2010.18080.x\">10.1111/j.1365-2966.2010.18080.x</a>","apa":"Wolcott-Green, J., &#38; Haiman, Z. (2011). Suppression of HD cooling in protogalactic gas clouds by Lyman-Werner radiation. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1111/j.1365-2966.2010.18080.x\">https://doi.org/10.1111/j.1365-2966.2010.18080.x</a>","ista":"Wolcott-Green J, Haiman Z. 2011. Suppression of HD cooling in protogalactic gas clouds by Lyman-Werner radiation. Monthly Notices of the Royal Astronomical Society. 412(4), 2603–2616.","ieee":"J. Wolcott-Green and Z. Haiman, “Suppression of HD cooling in protogalactic gas clouds by Lyman-Werner radiation,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 412, no. 4. Oxford University Press, pp. 2603–2616, 2011."},"publisher":"Oxford University Press","type":"journal_article","month":"04","scopus_import":"1","quality_controlled":"1","doi":"10.1111/j.1365-2966.2010.18080.x","publication":"Monthly Notices of the Royal Astronomical Society","year":"2011","publication_identifier":{"issn":["0035-8711"]},"oa":1,"extern":"1","_id":"17676","volume":412,"title":"Suppression of HD cooling in protogalactic gas clouds by Lyman-Werner radiation","intvolume":"       412","abstract":[{"text":"It has been shown that HD molecules can form efficiently in metal-free gas collapsing into massive protogalactic halos at high redshift. The resulting radiative cooling by HD can lower the gas temperature to that of the cosmic microwave background, T_CMB=2.7(1+z)K, significantly below the temperature of a few 100 K achievable via H_2-cooling alone, and thus reduce the masses of the first generation of stars. Here we consider the suppression of HD-cooling by UV irradiation in the Lyman-Werner (LW) bands. We include photo-dissociation of both H_2 and HD, and explicitly compute the self-shielding and shielding of both molecules by neutral hydrogen as well as the shielding of HD by H_2. We use a simplified dynamical collapse model, and follow the chemical and thermal evolution of the gas, in the presence of a UV background. We find that a LW flux of J_crit = 1e-22 erg/cm^2/sr/s/Hz is able to suppress HD cooling and thus prevent collapsing primordial gas from reaching temperatures below 100 K. The main reason for the lack of HD cooling for J>J_crit is the partial photo-dissociation of H_2, which prevents the gas from reaching sufficiently low temperatures (T<150K) for HD to become the dominant coolant; direct HD photo-dissociation is unimportant except for a narrow range of fluxes and column densities. Since the prevention of HD-cooling requires only partial H_2 photo-dissociation, the critical flux J_crit is modest, and is below the UV background required to reionize the universe at redshift z=10-20. We conclude that HD-cooling can reduce the masses of typical stars only in rare halos forming well before the epoch of reionization.","lang":"eng"}],"publication_status":"published","article_processing_charge":"No"}