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001     295125
005     20211110133410.0
024 7 _ |a arXiv:1111.3976
|2 arXiv
024 7 _ |a 10.3204/DESY-PROC-2011-04/sikivie_pierre
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024 7 _ |a inspire:946461
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037 _ _ |a PUBDB-2016-01073
088 1 _ |a arXiv:1111.3976
088 _ _ |a arXiv:1111.3976
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100 1 _ |a Erken, Ozgur
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111 2 _ |a 7th Patras Workshop on Axions, WIMPs and WISPs
|g AXION-WIMP 2011
|c Mykonos
|d 2011-06-27 - 2011-07-01
|w Greece
245 _ _ |a Axion BEC Dark Matter
260 _ _ |c 2011
300 _ _ |a 43-46
336 7 _ |a Conference Paper
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336 7 _ |a Internal Report
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336 7 _ |a INPROCEEDINGS
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520 _ _ |a Cold dark matter axions thermalize through gravitational self-interactions and form a Bose-Einstein condensate when the photon temperature reaches approximately 500 eV. Axion Bose-Einstein condensation provides an opportunity to distinguish axions from the other dark matter candidates on the basis of observation. The rethermalization of axions that are about to fall in a galactic potential well causes them to acquire net overall rotation, whereas ordinary cold dark matter falls in with an irrotational velocity field. The inner caustics of galactic halos are different in the two cases.
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588 _ _ |a Dataset connected to INSPIRE
650 _ 7 |a condensation: Bose-Einstein
|2 INSPIRE
650 _ 7 |a axion: dark matter
|2 INSPIRE
650 _ 7 |a dark matter: galaxy: halo
|2 INSPIRE
650 _ 7 |a photon: temperature
|2 INSPIRE
650 _ 7 |a galaxy: halo
|2 INSPIRE
650 _ 7 |a gravitation
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650 _ 7 |a rotation
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650 _ 7 |a velocity
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650 _ 7 |a WISP
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650 _ 7 |a WIMP
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693 _ _ |a HERA
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700 1 _ |a Sikivie, Pierre
|0 P:(DE-HGF)0
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700 1 _ |a Tam, Heywood
|0 P:(DE-HGF)0
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700 1 _ |a Yang, Qiaoli
|0 P:(DE-HGF)0
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773 _ _ |a 10.3204/DESY-PROC-2011-04/sikivie_pierre
787 0 _ |a Schumann, Marc et.al.
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|t Proceedings, 7th Patras Workshop on Axions, WIMPs and WISPs
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