Hostname: page-component-78c5997874-4rdpn Total loading time: 0 Render date: 2024-11-11T00:25:57.078Z Has data issue: false hasContentIssue false
  • English
  • Français

Dark Stars: Dark matter in the first stars leads to a new phase of stellar evolution

Published online by Cambridge University Press:  01 June 2008

Katherine Freese ,
Douglas Spolyar ,
Anthony Aguirre ,
Peter Bodenheimer ,
Paolo Gondolo ,
J. A. Sellwood  and
Naoki Yoshida
Katherine Freese
Affiliation:
Michigan Center for Theoretical Physics, University of Michigan, Ann Arbor, MI 48109, USA email: ktfreese@umich.edu
Douglas Spolyar
Affiliation:
Dept. of Physics, University of California, Santa Cruz, CA 95064, USA email: dspolyar@physics.ucsc.edu, aguirre@scipp.ucsc.edu
Anthony Aguirre
Affiliation:
Dept. of Physics, University of California, Santa Cruz, CA 95064, USA email: dspolyar@physics.ucsc.edu, aguirre@scipp.ucsc.edu
Peter Bodenheimer
Affiliation:
Dept. of Astronomy, University of California, Santa Cruz, CA 95064, USA email: peter@ucolick.org
Paolo Gondolo
Affiliation:
Physics Dept., University of Utah, Salt Lake City, UT 84112, USA email: paolo@physics.utah.edu
J. A. Sellwood
Affiliation:
Dept. of Physics and Astronomy, Rutgers Univ., Piscataway, NJ 08854, USA email: sellwood@physics.rutgers.edu
Naoki Yoshida
Affiliation:
Inst. for the Physics and Math. of the Universe, Univ. of Tokyo, Kashiwa, Chiba, Japan email: nyoshida@a.phys.nagoya-u-ac.jp
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The first phase of stellar evolution in the history of the universe may be Dark Stars, powered by dark matter heating rather than by fusion. Weakly interacting massive particles, which are their own antiparticles, can annihilate and provide an important heat source for the first stars in the the universe. This talk presents the story of these Dark Stars. We make predictions that the first stars are very massive (~800M⊙), cool (6000 K), bright (~106L⊙), long-lived (~106 years), and probable precursors to (otherwise unexplained) supermassive black holes. Later, once the initial DM fuel runs out and fusion sets in, DM annihilation can predominate again if the scattering cross section is strong enough, so that a Dark Star is born again.

Keywords

cosmology: dark matterstars: evolutionstars: fundamental parameters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Issue S255: Low-Metallicity Star Formation: From the First Stars to Dwarf Galaxies , June 2008 , pp. 56 - 60
Copyright
Copyright © International Astronomical Union 2008

References

Spolyar, D., Freese, K., & Gondolo, P. astro-ph/0705.0521, 2008, Phys. Rev. Lett., 100, 051101CrossRefGoogle Scholar
Freese, K., Gondolo, P., & Spolyar, D. 2008, AIP Conf.Proc., 990, 42CrossRefGoogle Scholar
Ripamonti, E. & Abel, T. astro-ph/0507130.Google Scholar
Barkana, R. & Loeb, A. 2001, Phys. Rep., 349, 125CrossRefGoogle Scholar
Bromm, V. & Larson, R. B. 2004, ARAA, 42, 79CrossRefGoogle Scholar
Yoshida, N., Omukai, K., Hernquist, L., & Abel, T. 2006, ApJ, 652, 6CrossRefGoogle Scholar
Navarro, J. F., Frenk, C. S., & White, S. D. M. 1996, ApJ, 462, 563CrossRefGoogle Scholar
Blumenthal, G. R., Faber, S. M., Flores, R., & Primack, J. R. 1986, ApJ, 301, 27CrossRefGoogle Scholar
Abel, T., Bryan, G. L., & Norman, M. L. 2002, Science, 295, 93CrossRefGoogle Scholar
Gao, L., Abel, T., Frenk, C. S., Jenkins, A., Springel, V., & Yoshida, N. 2007, MNRAS. 378, 449CrossRefGoogle Scholar
Natarajan, A., Tan, J., & O'Shea, B. 2008, arXiv:0807.3769 [astro-ph]Google Scholar
Freese, K., Gondolo, P., Sellwood, J., & Spolyar, D. 2008, arxiv:0805.3540 [astro-ph]Google Scholar
Ripamonti, E., Mapelli, M., & Ferrara, A. 2007, MNRAS, 375, 1399CrossRefGoogle Scholar
Hollenbach, D. & McKee, C. F. 1979, ApJ Suppl., 41, 555CrossRefGoogle Scholar
Yoshida, N., Freese, K., Gondolo, P., & Spolyar, D. 2008, in preparationGoogle Scholar
Freese, K., Bodenheimer, P., Spolyar, D., & Gondolo, P. 2008, arxiv:0806.0617 [astro-ph]Google Scholar
Heger, A. & Woosley, A. 2002, ApJ, 567, 532CrossRefGoogle Scholar
Li, Y. X. et al. 2007, ApJ, 665, 187CrossRefGoogle Scholar
Pelupessy, F. I., Matteo, T. Di, & Ciardi, B. 2007, arXiv:astro-ph/0703773.Google Scholar
Freese, K., Spolyar, D., & Aguirre, A. 2008, arXiv:0802.1724 [astro-ph]CrossRefGoogle Scholar
Iocco, F. 2008, ApJ Letters, 677, 1CrossRefGoogle Scholar
Iocco, F., Bressan, A., Ripamonti, E., Schneider, R., Ferrara, A., & Marigo, P. 2008, arXiv:0805.4016Google Scholar
Taoso, M., Bertone, G., Meynet, G., & Ekstrom, S. 2008, arXiv:0806.2681 [astro-ph]Google Scholar
Yoon, S., Iocco, F., & Akiyama, S. 2008, arxiv:0806.2662 [astro-ph]Google Scholar