Particle dark energy
We explore the physics of a gas of particles interacting with a condensate that spontaneously breaks Lorentz invariance. The equation of state of this gas varies from 1/3 to less than -1 and can lead to the observed cosmic acceleration without requiring a vacuum energy. The particles are always stab...
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| Veröffentlicht in: | Physical review. D, Particles and fields Particles and fields, 2006-02, Vol.73 (4), Article 043520 |
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| container_title | Physical review. D, Particles and fields |
| container_volume | 73 |
| creator | DeDeo, Simon |
| description | We explore the physics of a gas of particles interacting with a condensate that spontaneously breaks Lorentz invariance. The equation of state of this gas varies from 1/3 to less than -1 and can lead to the observed cosmic acceleration without requiring a vacuum energy. The particles are always stable. In our particular class of models these particles are fermions with a chiral coupling to the condensate. They may behave as relativistic matter at early times, produce a brief period where they dominate the expansion with w |
| doi_str_mv | 10.1103/PhysRevD.73.043520 |
| format | Article |
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The equation of state of this gas varies from 1/3 to less than -1 and can lead to the observed cosmic acceleration without requiring a vacuum energy. The particles are always stable. In our particular class of models these particles are fermions with a chiral coupling to the condensate. They may behave as relativistic matter at early times, produce a brief period where they dominate the expansion with w<0 today, and behave as matter at late time. 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The equation of state of this gas varies from 1/3 to less than -1 and can lead to the observed cosmic acceleration without requiring a vacuum energy. The particles are always stable. In our particular class of models these particles are fermions with a chiral coupling to the condensate. They may behave as relativistic matter at early times, produce a brief period where they dominate the expansion with w<0 today, and behave as matter at late time. There are no small parameters in our models, which generically lead to dark energy clustering and, depending on the choice of parameters, smoothing of small scale power.</description><subject>ACCELERATION</subject><subject>CHIRALITY</subject><subject>COSMOLOGY</subject><subject>COUPLING</subject><subject>EQUATIONS OF STATE</subject><subject>EXPANSION</subject><subject>FERMIONS</subject><subject>LORENTZ INVARIANCE</subject><subject>NONLUMINOUS MATTER</subject><subject>PARTICLE IDENTIFICATION</subject><subject>PHYSICS OF ELEMENTARY PARTICLES AND FIELDS</subject><subject>RELATIVISTIC RANGE</subject><issn>1550-7998</issn><issn>0556-2821</issn><issn>1550-2368</issn><issn>1089-4918</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2006</creationdate><recordtype>article</recordtype><recordid>eNo1j0FLxDAQhYMouK7ePHla8NyaZJpOc5TVVWHBRfQcmsnUra6tJEXov3el6-k9eB8PPiGulMyVknCz2Y7phX_ucoRcFmC0PBIzZYzMNJTV8aGjtdWpOEvpQ0rQJeJMXG7qOLS040Wo4-eCO47v47k4aepd4otDzsXb6v51-Zitnx-elrfrjDSaISuKSnOpLRWFD0GGskLP3qMG0mSoqZWnsmGLjQGrgjWMnsBWSu83Hxjm4nr67dPQukTtwLSlvuuYBqclYomAe0pPFMU-pciN-47tVx1Hp6T7s3f_9g7BTfbwC0ELTjI</recordid><startdate>20060201</startdate><enddate>20060201</enddate><creator>DeDeo, Simon</creator><scope>AAYXX</scope><scope>CITATION</scope><scope>OTOTI</scope></search><sort><creationdate>20060201</creationdate><title>Particle dark energy</title><author>DeDeo, Simon</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c275t-4482e629c44bdd0d687bebb723c2c5cfa1bc6fe97f5391d95e7bc39812cfabde3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2006</creationdate><topic>ACCELERATION</topic><topic>CHIRALITY</topic><topic>COSMOLOGY</topic><topic>COUPLING</topic><topic>EQUATIONS OF STATE</topic><topic>EXPANSION</topic><topic>FERMIONS</topic><topic>LORENTZ INVARIANCE</topic><topic>NONLUMINOUS MATTER</topic><topic>PARTICLE IDENTIFICATION</topic><topic>PHYSICS OF ELEMENTARY PARTICLES AND FIELDS</topic><topic>RELATIVISTIC RANGE</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>DeDeo, Simon</creatorcontrib><collection>CrossRef</collection><collection>OSTI.GOV</collection><jtitle>Physical review. D, Particles and fields</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>DeDeo, Simon</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Particle dark energy</atitle><jtitle>Physical review. D, Particles and fields</jtitle><date>2006-02-01</date><risdate>2006</risdate><volume>73</volume><issue>4</issue><artnum>043520</artnum><issn>1550-7998</issn><issn>0556-2821</issn><eissn>1550-2368</eissn><eissn>1089-4918</eissn><abstract>We explore the physics of a gas of particles interacting with a condensate that spontaneously breaks Lorentz invariance. The equation of state of this gas varies from 1/3 to less than -1 and can lead to the observed cosmic acceleration without requiring a vacuum energy. The particles are always stable. In our particular class of models these particles are fermions with a chiral coupling to the condensate. They may behave as relativistic matter at early times, produce a brief period where they dominate the expansion with w<0 today, and behave as matter at late time. There are no small parameters in our models, which generically lead to dark energy clustering and, depending on the choice of parameters, smoothing of small scale power.</abstract><cop>United States</cop><doi>10.1103/PhysRevD.73.043520</doi></addata></record> |
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| identifier | ISSN: 1550-7998 |
| ispartof | Physical review. D, Particles and fields, 2006-02, Vol.73 (4), Article 043520 |
| issn | 1550-7998 0556-2821 1550-2368 1089-4918 |
| language | eng |
| recordid | cdi_osti_scitechconnect_20776737 |
| source | American Physical Society Journals |
| subjects | ACCELERATION CHIRALITY COSMOLOGY COUPLING EQUATIONS OF STATE EXPANSION FERMIONS LORENTZ INVARIANCE NONLUMINOUS MATTER PARTICLE IDENTIFICATION PHYSICS OF ELEMENTARY PARTICLES AND FIELDS RELATIVISTIC RANGE |
| title | Particle dark energy |
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