Dark Stars: Improved Models And First Pulsation Results

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dc.contributor.utaustinauthorMontgomery, Michael H.en_US
dc.contributor.utaustinauthorWinget, D. E.en_US
dc.creatorRindler-Daller, T.en_US
dc.creatorMontgomery, Michael H.en_US
dc.creatorFreese, K.en_US
dc.creatorWinget, D. E.en_US
dc.creatorPaxton, B.en_US
dc.date.accessioned2016-04-28T19:41:28Z
dc.date.available2016-04-28T19:41:28Z
dc.date.issued2015-02en
dc.description.abstractWe use the stellar evolution code MESA to study dark stars (DSs). DSs, which are powered by dark matter (DM) self-annihilation rather than by nuclear fusion, may be the first stars to form in the universe. We compute stellar models for accreting DSs with masses up to 10(6) M-circle dot. The heating due to DM annihilation is self-consistently included, assuming extended adiabatic contraction of DM within the minihalos in which DSs form. We find remarkably good overall agreement with previous models, which assumed polytropic interiors. There are some differences in the details, with positive implications for observability. We found that, in the mass range of 10(4)-10(5) M-circle dot, our DSs are hotter by a factor of 1.5 than those in Freese et al., are smaller in radius by a factor of 0.6, denser by a factor of three to four, and more luminous by a factor of two. Our models also confirm previous results, according to which supermassive DSs are very well approximated by (n = 3)-polytropes. We also perform a first study of DS pulsations. Our DS models have pulsation modes with timescales ranging from less than a day to more than two years in their rest frames, at z similar to 15, depending on DM particle mass and overtone number. Such pulsations may someday be used to identify bright, cool objects uniquely as DSs; if properly calibrated, they might, in principle, also supply novel standard candles for cosmological studies.en_US
dc.description.departmentAstronomyen_US
dc.description.sponsorshipDepartment of Energyen_US
dc.description.sponsorshipDOE-FG02-95ER40899en_US
dc.description.sponsorshipMichigan Center for Theoretical Physics at the University of Michigan, Ann Arboren_US
dc.description.sponsorshipNational Science Foundation AST-0909107, AST-1312983, PHYS-1066293en_US
dc.description.sponsorshipNASA NNX12AC96Gen_US
dc.identifierdoi:10.15781/T27N7F
dc.identifier.Filename2015_02_darkstars.pdfen_US
dc.identifier.citationRindler-Daller, Tanja, Michael H. Montgomery, Katherine Freese, Donald E. Winget, and Bill Paxton. "Dark Stars: Improved Models and First Pulsation Results." The Astrophysical Journal, Vol. 799, No. 2 (Feb., 2015): 210.en_US
dc.identifier.doi10.1088/0004-637x/799/2/210en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/2152/35111
dc.language.isoEnglishen_US
dc.relation.ispartofen_US
dc.relation.ispartofserialAstrophysical Journalen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.rights.restrictionOpenen_US
dc.subjectastroparticle physicsen_US
dc.subjectdark ages, reionization, first starsen_US
dc.subjectdarken_US
dc.subjectmatteren_US
dc.subjectstars: evolutionen_US
dc.subjectstars: oscillations (including pulsations)en_US
dc.subjectstellar astrophysics mesaen_US
dc.subjectpopulation iii starsen_US
dc.subjectmatter annihilationen_US
dc.subjectprimordial gasen_US
dc.subjectevolutionen_US
dc.subjectaccretionen_US
dc.subjectfragmentationen_US
dc.subjectbinariesen_US
dc.subjectuniverseen_US
dc.subjectmodulesen_US
dc.subjectastronomy & astrophysicsen_US
dc.titleDark Stars: Improved Models And First Pulsation Resultsen_US
dc.typeArticleen_US

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