376:. The dark matter can be described as a Bose–Einstein condensate of the ultralight quanta of the field and as boson stars. The enormous Compton wavelength of these particles prevents structure formation on small, subgalactic scales, which is a major problem in traditional cold dark matter models. The collapse of initial over-densities is studied in the references. There are not many models in which we consider dark matter as the scalar field.
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The occupation number of these particles is so huge that we can consider the wave nature of these particles in the classical description. To satisfy Pauli's exclusion principle the particle must be bosons especially spin zero (scalar) particles. hence these ultra-light dark matter would be more like
128:), and for some reasonable estimates of particle mass and density of dark matter there is no point talking about the individual particles' positions and momenta. By some dynamical measurements, we can deduce that the mass density of the dark matter is about
120:. In this picture the dark matter consists of an ultralight particle with a mass of ~10 eV when there is no self-interaction. If there is a self-interaction a wider mass range is allowed. The uncertainty in position of a particle is larger than its
359:
76:
The universe may be accelerating, fueled perhaps by a cosmological constant or some other field possessing long range 'repulsive' effects. A model must predict the correct form for the large scale clustering spectrum, account for
553:. Contributors: Reginald T. Cahill, F. Siddhartha Guzman, N. Hiotelis, A.A. Kirillov, V.E. Kuzmichev, V.V. Kuzmichev, A. Miyazaki, Yu. A. Shchekinov, L. Arturo Urena-Lopez, E.I. Vorobyov. Nova Publishers. p. 40.
573:
Galaxies are not scattered about the universe in a random way, but rather form an intricate network of filaments, sheets, and clusters. How these large-scale structures formed is at the root of many key questions in
380:-like particle (ALP) in string theory can be considered as a model of scalar field dark matter, as its mass density satisfies the relic density of the dark matter. The most common production mechanism of ALP is
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92:. The modeled evolution of the universe includes a large amount of unknown matter and energy in order to agree with such observations. This energy density has two components:
45:(intergalactic gas and about 0.1% neutrinos and 0.04% supermassive black holes). Ordinary matter is uncommon. Modeled after Ostriker and Steinhardt. For more information, see
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Alcubierre, Miguel; Guzmán, F. Siddhartha; Matos, Tonatiuh; Núñez, Darío; Ureña-López, L. Arturo; Wiederhold, Petra (2002). "Galactic collapse of scalar field dark matter".
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100:. Each contributes to the theory of the origination of galaxies and the expansion of the universe. The universe must have a critical density, a density not explained by
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is the dispersion velocity of the halo. The average number of the particles in cubic volume having the dimension equal to the de
Broglie wavelength,
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Guzmán, F. Siddhartha; Ureña-López, L. Arturo (2004). "Evolution of the Schrödinger-Newton system for a self-gravitating scalar field".
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Matos, Tonatiuh; Ureña-López, L. Arturo (2001). "Further analysis of a cosmological model with quintessence and scalar dark matter".
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Matos, Tonatiuh; Ureña-López, L. Arturo (2000). "Quintessence and scalar dark matter in the
Universe". Letter to the Editor.
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Bernal, Argelia; Guzmán, F. Siddhartha (2006). "Scalar field dark matter: Nonspherical collapse and late-time behavior".
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Guzmán, F. Siddhartha; Ureña-López, L. Arturo (2006). "Gravitational
Cooling of Self-gravitating Bose Condensates".
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Baldeschi, M. R.; Gelmini, G. B.; Ruffini, R. (10 March 1983). "On massive fermions and bosons in galactic halos".
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Membrado, M.; Pacheco, A. F.; Sañudo, J. (1 April 1989). "Hartree solutions for the self-Yukawian boson sphere".
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Sin, Sang-Jin; Urena-Lopez, L.A. (1994). "Late-time phase transition and the galactic halo as a Bose liquid".
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354:{\displaystyle N_{db}=\left({\frac {34eV}{m}}\right)^{4}\left({\frac {250km/s}{v}}\right)^{3}}
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Pie chart showing the fractions of energy in the universe contributed by different sources.
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Classical, minimally coupled, scalar field postulated to account for the inferred dark matter
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Sahni, Varun; Wang, Limin (2000). "New cosmological model of quintessence and dark matter".
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The dark matter can be modeled as a scalar field using two fitted parameters, mass and
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is a classical, minimally coupled, scalar field postulated to account for the inferred
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515: – Hypothetical form of cold dark matter proposed to solve the cuspy halo problem
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anisotropies on large and intermediate angular scales, and provide agreement with the
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This dark matter model is also known as BEC dark matter or wave dark matter.
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Lee, Jae-Weon; Koh, In-Gyu (1996). "Galactic halos as boson stars".
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and ultra-light axion are examples of scalar field dark matter.
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satisfies with the relic abundance of observed dark matter.
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Pages displaying short descriptions of redirect targets
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438:{\displaystyle (10^{-22}-10^{-20})\ eV}
471:Minimal Supersymmetric Standard Model
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462:Weakly interacting massive particles
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212:{\displaystyle \lambda =2\pi /mv}
172:{\displaystyle 0.4\ GeV\ cm^{-3}}
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364:a wave than a particle, and the
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1882:Galaxy formation and evolution
550:Trends in Dark Matter Research
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384:. Which shows the mass around
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948:Classical and Quantum Gravity
664:Classical and Quantum Gravity
1304:Self-interacting dark matter
1164:Annu. Rev. Astron. Astrophys
606:10.1016/0370-2693(83)90688-3
247:{\displaystyle \lambda ^{3}}
83:luminosity distance relation
1462:Navarro–Frenk–White profile
1452:Massive compact halo object
1447:Mass dimension one fermions
978:10.1088/0264-9381/19/19/314
694:10.1088/0264-9381/17/13/101
79:cosmic microwave background
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1137:10.1103/PhysRevD.74.063504
1031:10.1103/PhysRevD.69.124033
800:10.1103/PhysRevD.62.103517
747:10.1103/PhysRevD.63.063506
547:J. Val Blain, ed. (2005).
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1054:The Astrophysical Journal
1467:Scalar field dark matter
1309:Scalar field dark matter
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856:10.1103/PhysRevD.53.2236
641:10.1103/PhysRevA.39.4207
535:New Light on Dark Matter
62:scalar field dark matter
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1332:Hypothetical particles
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633:1989PhRvA..39.4207M
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1402:Cuspy halo problem
1220:Scaled-Up Darkness
1160:"Wave Dark Matter"
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1158:Hui, Lam (2021).
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1001:Physical Review D
954:(19): 5017–5024.
887:Physical Review D
826:Physical Review D
770:Physical Review D
717:Physical Review D
621:Physical Review A
586:Physics Letters B
560:978-1-59454-248-0
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112:Scalar field
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55:astrophysics
52:
42:
38:
34:
1960:Dark matter
1872:Dark energy
1836:HE0450-2958
1478:experiments
1412:Dark galaxy
1395:and objects
1349:Dark photon
1267:dark matter
1258:Dark matter
670:(13): L75.
372:, possibly
370:bose liquid
126:light years
98:dark energy
66:dark matter
1949:Categories
1867:Antimatter
1826:Potential
1554:DAMA/LIBRA
1407:Dark fluid
1364:Neutralino
1177:2101.11735
574:cosmology.
520:References
477:Neutralino
374:superfluid
104:(ordinary
90:supernovae
72:Background
19:See also:
1851:VIRGOHI21
1808:MultiDark
1715:detection
1599:EDELWEISS
1487:detection
1432:Dark star
1202:231719700
1145:119542259
933:119415858
808:119480411
416:−
408:−
400:−
236:λ
196:π
187:λ
162:−
108:) alone.
59:cosmology
1921:Category
1713:Indirect
1569:DarkSide
1559:DAMA/NaI
1393:Theories
1265:Forms of
1039:53064807
986:26660029
925:10018007
872:16914311
864:10020213
755:55583802
702:44042014
456:See also
87:redshift
1933:Commons
1860:Related
1792:VERITAS
1767:IceCube
1727:ANTARES
1679:TREX-DM
1664:ROSEBUD
1654:PICASSO
1182:Bibcode
1170:: 247.
1125:Bibcode
1092:1863630
1072:Bibcode
1019:Bibcode
966:Bibcode
905:Bibcode
844:Bibcode
788:Bibcode
735:Bibcode
682:Bibcode
649:9901751
629:Bibcode
594:Bibcode
219:, here
1787:PAMELA
1722:AMS-02
1704:ZEPLIN
1674:SIMPLE
1649:PandaX
1644:NEWS-G
1639:NEWAGE
1604:EURECA
1584:DM-Ice
1574:DARWIN
1539:CRESST
1529:COSINE
1524:CoGeNT
1485:Direct
1476:Search
1200:
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106:matter
1813:PVLAS
1772:MAGIC
1752:Fermi
1747:DAMPE
1737:CALET
1699:XMASS
1694:XENON
1684:UKDMC
1669:SABRE
1634:NAIAD
1629:MIMAC
1624:MACRO
1594:DRIFT
1589:DMTPC
1564:DAMIC
1544:CUORE
1534:COUPP
1519:CLEAN
1499:ANAIS
1344:Axion
1339:Axino
1198:S2CID
1172:arXiv
1141:S2CID
1115:arXiv
1088:S2CID
1062:arXiv
1035:S2CID
1009:arXiv
982:S2CID
956:arXiv
929:S2CID
895:arXiv
868:S2CID
834:arXiv
804:S2CID
778:arXiv
751:S2CID
725:arXiv
698:S2CID
672:arXiv
483:Axion
378:Axion
1782:OGLE
1762:HESS
1757:HAWC
1742:CAST
1732:ATIC
1689:WARP
1659:PICO
1609:KIMS
1579:DEAP
1514:CDMS
1509:CDEX
1504:ArDM
1494:ADMX
1384:WISP
1379:WIMP
1374:SIMP
921:PMID
860:PMID
645:PMID
555:ISBN
96:and
57:and
47:NASA
23:and
1777:MOA
1614:LUX
1354:LSP
1190:doi
1133:doi
1080:doi
1058:645
1027:doi
974:doi
913:doi
852:doi
796:doi
743:doi
690:doi
637:doi
602:doi
590:122
319:250
136:0.4
53:In
1951::
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270:b
267:d
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207:v
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190:=
165:3
158:m
154:c
148:V
145:e
142:G
49:.
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