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Light dark matter

December 15, 2023

See also: Lambda-CDM model and Galaxy formation

Light dark matter, in astronomy and cosmology, are dark matter weakly interacting massive particles (WIMPS) candidates with masses less than 1 GeV.[1] These particles are heavier than warm dark matter and hot dark matter, but are lighter than the traditional forms of cold dark matter, such as Massive Compact Halo Objects (MACHOs). The Lee-Weinberg bound[2] limits the mass of the favored dark matter candidate, WIMPs, that interact via the weak interaction to GeV. This bound arises as follows. The lower the mass of WIMPs is, the lower the annihilation cross section, which is of the order , where m is the WIMP mass and M the mass of the Z-boson. This means that low mass WIMPs, which would be abundantly produced in the early universe, freeze out (i.e. stop interacting) much earlier and thus at a higher temperature, than higher mass WIMPs. This leads to a higher relic WIMP density. If the mass is lower than GeV the WIMP relic density would overclose the universe.

Some of the few loopholes allowing one to avoid the Lee-Weinberg bound without introducing new forces below the electroweak scale have been ruled out by accelerator experiments (i.e. CERN, Tevatron), and in decays of B mesons.[3]

A viable way of building light dark matter models is thus by postulating new light bosons. This increases the annihilation cross section and reduces the coupling of dark matter particles to the Standard Model making them consistent with accelerator experiments.[4][5][6]

Current methods to search for light dark matter particles include direct detection through electron recoil.

Motivation edit

In recent years, light dark matter has become popular due in part to the many benefits of the theory. Sub-GeV dark matter has been used to explain the positron excess in the Galactic Center observed by INTEGRAL, excess gamma rays from the Galactic Center[7] and extragalactic sources. It has also been suggested that light dark matter may explain a small discrepancy in the measured value of the fine structure constant in different experiments.[8] Furthermore, the lack of dark matter signals in higher energy ranges in direct detection experiments incentivizes sub-GeV searches.

Theoretical Models for Light Dark Matter edit

Due to the constraints placed on the mass of WIMPs in the popular freeze out model which predict WIMP masses greater than 2 GeV, the freeze out model must be altered to allow for lower mass dark matter particles.[9]

Scalar Dark Matter edit

The Lee-Weinberg limit, which restricts the mass of dark matter particles to >2 GeV may not apply in two special cases where dark matter is a scalar particle.[2]

The first case requires that the scalar dark matter particle is coupled with a massive fermion. This model rules out dark matter particles less than 100 MeV because observations of gamma ray production do not align with theoretical predictions for particles in this mass range. This discrepancy may be resolved by requiring an asymmetry between the dark matter particles and antiparticles, as well as adding new particles.[4]

The second case predicts that the scalar dark matter particle is coupled with a new gauge boson. The production of gamma rays due to annihilation in this case is predicted to be very low.[4]

Freeze In Model edit

The thermal freeze in model proposes that dark matter particles were very weakly interacting shortly after the Big Bang such that they were essentially decoupled from the plasma. Furthermore, their initial abundance was small. Dark matter production occurs predominantly when the temperature of the plasma falls under the mass of the dark matter particle itself. This is in contrast to the thermal freeze out theory, in which the initial abundance of dark matter was large, and differentiation into lighter particles decreases and eventually stops as the temperature of the plasma decreases.[10]

The freeze in model allows for dark matter particles well under the 2 GeV mass limit to exist.[11]

Asymmetric Dark Matter edit

Observations show that the density of dark matter is about 5 times the density of baryonic matter. Asymmetric dark matter theories attempt to explain this relationship by suggesting that the ratio between the number densities of particles and antiparticles is the same in baryonic matter as it is in dark matter. This further implies that the mass of dark matter is close to 5 times the mass of baryonic matter, placing the mass of dark matter in the few GeV range.[12]

Experiments edit

In general, the methods for detecting dark matter which apply to all heavier dark matter candidates also apply to light dark matter. These methods include direct detection and indirect detection. Dark matter particles with masses lighter than 1 GeV can be directly detected by searching for electron recoils. The greatest difficulty in using this method is creating a detector with a low enough threshold energy for detection while also minimizing background signals. Electron beam dump experiments can also be used to search for light dark matter particles.[13]

XENON10 edit

XENON10 is a liquid xenon detector that searches for and places limits on the mass of dark matter by directly detecting electron recoil. This experiment placed the first sub GeV limits on the mass of dark matter using direct detection in 2012.[14]

SENSEI edit

SENSEI is a silicon detector capable of measuring the electronic recoil of a dark matter particle between 500 keV and 4 MeV using CCD technology.[15] The experiment has been working to place further rule out possible mass ranges of dark matter below 1 GeV, with its most recent results being published in October 2020.[16]

See also edit

References edit

  1. ^ Cassé, M.; Fayet, P. (4–9 July 2005). Light Dark Matter. 21st IAP Colloquium "Mass Profiles and Shapes of Cosmological Structures". Paris. arXiv:astro-ph/0510490. Bibcode:2006EAS....20..201C. doi:10.1051/eas:2006072.
  2. ^ a b Lee B.W.; Weinberg S. (1977). "Cosmological Lower Bound on Heavy-Neutrino Masses". Physical Review Letters. 39 (4): 165–168. Bibcode:1977PhRvL..39..165L. doi:10.1103/PhysRevLett.39.165.
  3. ^ Bird, C.; Kowalewski, R.; Pospelov, M. (2006). "Dark matter pair-production in b → s transitions". Mod. Phys. Lett. A. 21 (6): 457–478. arXiv:hep-ph/0601090. Bibcode:2006MPLA...21..457B. doi:10.1142/S0217732306019852. S2CID 119072470.
  4. ^ a b c Boehm, C.; Fayet, P. (2004). "Scalar Dark Matter candidates". Nuclear Physics B. 683 (1–2): 219–263. arXiv:hep-ph/0305261. Bibcode:2004NuPhB.683..219B. doi:10.1016/j.nuclphysb.2004.01.015. S2CID 17516917.
  5. ^ Boehm, C.; Fayet, P.; Silk, J. (2004). "Light and Heavy Dark Matter Particles". Physical Review D. 69 (10): 101302. arXiv:hep-ph/0311143. Bibcode:2004PhRvD..69j1302B. doi:10.1103/PhysRevD.69.101302. S2CID 119465958.
  6. ^ Boehm, C. (2004). "Implications of a new light gauge boson for neutrino physics". Physical Review D. 70 (5): 055007. arXiv:hep-ph/0405240. Bibcode:2004PhRvD..70e5007B. doi:10.1103/PhysRevD.70.055007. S2CID 41227342.
  7. ^ Beacom, J.F.; Bell, N.F.; Bertone, G. (2005). "Gamma-Ray Constraint on Galactic Positron Production by MeV Dark Matter". Physical Review Letters. 94 (17): 171301. arXiv:astro-ph/0409403. Bibcode:2005PhRvL..94q1301B. doi:10.1103/PhysRevLett.94.171301. PMID 15904276. S2CID 20043249.
  8. ^ Boehm, C.; Ascasibar, Y. (2004). "More evidence in favour of Light Dark Matter particles?". Physical Review D. 70 (11): 115013. arXiv:hep-ph/0408213. Bibcode:2004PhRvD..70k5013B. doi:10.1103/PhysRevD.70.115013. S2CID 119363575.
  9. ^ Roszkowski, Leszek; Sessolo, Enrico Maria; Trojanowski, Sebastian (2018-05-21). "WIMP dark matter candidates and searches—current status and future prospects". Reports on Progress in Physics. 81 (6): 066201. arXiv:1707.06277. Bibcode:2018RPPh...81f6201R. doi:10.1088/1361-6633/aab913. ISSN 0034-4885. PMID 29569575. S2CID 4166809.
  10. ^ Hall, Lawrence J.; Jedamzik, Karsten; March-Russell, John; West, Stephen M. (2010). "Freeze-In Production of FIMP Dark Matter" (PDF). Journal of High Energy Physics. 2010 (3): 80. arXiv:0911.1120. Bibcode:2010JHEP...03..080H. doi:10.1007/JHEP03(2010)080. S2CID 119166813 – via Springer.
  11. ^ Dvorkin, Cora; Lin, Tongyan; Schutz, Katelin (2021-09-09). "The cosmology of sub-MeV dark matter freeze-in". Physical Review Letters. 127 (11): 111301. arXiv:2011.08186. Bibcode:2021PhRvL.127k1301D. doi:10.1103/PhysRevLett.127.111301. ISSN 0031-9007. PMID 34558939. S2CID 226976117.
  12. ^ Zurek, Kathryn M. (2014-04-20). "Asymmetric Dark Matter: Theories, signatures, and constraints". Physics Reports. Asymmetric Dark Matter: Theories, signatures, and constraints. 537 (3): 91–121. arXiv:1308.0338. Bibcode:2014PhR...537...91Z. doi:10.1016/j.physrep.2013.12.001. ISSN 0370-1573. S2CID 118542568.
  13. ^ Diamond, Miriam D.; Schuster, Philip (2013-11-27). "Searching for Light Dark Matter with the SLAC Millicharge Experiment". Physical Review Letters. 111 (22): 221803. arXiv:1307.6861. Bibcode:2013PhRvL.111v1803D. doi:10.1103/PhysRevLett.111.221803. ISSN 0031-9007. PMID 24329439. S2CID 7344960.
  14. ^ Essig, Rouven; Manalaysay, Aaron; Mardon, Jeremy; Sorensen, Peter; Volansky, Tomer (2012-07-12). "First Direct Detection Limits on Sub-GeV Dark Matter from XENON10". Physical Review Letters. 109 (2): 021301. arXiv:1206.2644. Bibcode:2012PhRvL.109b1301E. doi:10.1103/PhysRevLett.109.021301. ISSN 0031-9007. PMID 23030151. S2CID 14131974.
  15. ^ Crisler, Michael; Essig, Rouven; Estrada, Juan; Fernandez, Guillermo; Tiffenberg, Javier; Haro, Miguel Sofo; Volansky, Tomer; Yu, Tien-Tien; SENSEI Collaboration (2018-08-08). "SENSEI: First Direct-Detection Constraints on Sub-GeV Dark Matter from a Surface Run". Physical Review Letters. 121 (6): 061803. arXiv:1804.00088. Bibcode:2018PhRvL.121f1803C. doi:10.1103/PhysRevLett.121.061803. ISSN 0031-9007. PMID 30141688. S2CID 52077932.
  16. ^ Barak, Liron; Bloch, Itay M.; Cababie, Mariano; Cancelo, Gustavo; Chaplinsky, Luke; Chierchie, Fernando; Crisler, Michael; Drlica-Wagner, Alex; Essig, Rouven; Estrada, Juan; Etzion, Erez (2020-10-20). "SENSEI: Direct-Detection Results on sub-GeV Dark Matter from a New Skipper CCD". Physical Review Letters. 125 (17): 171802. arXiv:2004.11378. Bibcode:2020PhRvL.125q1802B. doi:10.1103/PhysRevLett.125.171802. hdl:11336/138737. ISSN 0031-9007. PMID 33156657. S2CID 216144756.

Further reading edit

December 15, 2023
light, dark, matter, also, lambda, model, galaxy, formation, astronomy, cosmology, dark, matter, weakly, interacting, massive, particles, wimps, candidates, with, masses, less, than, these, particles, heavier, than, warm, dark, matter, dark, matter, lighter, t. See also Lambda CDM model and Galaxy formation Light dark matter in astronomy and cosmology are dark matter weakly interacting massive particles WIMPS candidates with masses less than 1 GeV 1 These particles are heavier than warm dark matter and hot dark matter but are lighter than the traditional forms of cold dark matter such as Massive Compact Halo Objects MACHOs The Lee Weinberg bound 2 limits the mass of the favored dark matter candidate WIMPs that interact via the weak interaction to 2 displaystyle approx 2 GeV This bound arises as follows The lower the mass of WIMPs is the lower the annihilation cross section which is of the order m 2 M 4 displaystyle approx m 2 M 4 where m is the WIMP mass and M the mass of the Z boson This means that low mass WIMPs which would be abundantly produced in the early universe freeze out i e stop interacting much earlier and thus at a higher temperature than higher mass WIMPs This leads to a higher relic WIMP density If the mass is lower than 2 displaystyle sim 2 GeV the WIMP relic density would overclose the universe Some of the few loopholes allowing one to avoid the Lee Weinberg bound without introducing new forces below the electroweak scale have been ruled out by accelerator experiments i e CERN Tevatron and in decays of B mesons 3 A viable way of building light dark matter models is thus by postulating new light bosons This increases the annihilation cross section and reduces the coupling of dark matter particles to the Standard Model making them consistent with accelerator experiments 4 5 6 Current methods to search for light dark matter particles include direct detection through electron recoil Contents 1 Motivation 2 Theoretical Models for Light Dark Matter 2 1 Scalar Dark Matter 2 2 Freeze In Model 2 3 Asymmetric Dark Matter 3 Experiments 3 1 XENON10 3 2 SENSEI 4 See also 5 References 6 Further readingMotivation editIn recent years light dark matter has become popular due in part to the many benefits of the theory Sub GeV dark matter has been used to explain the positron excess in the Galactic Center observed by INTEGRAL excess gamma rays from the Galactic Center 7 and extragalactic sources It has also been suggested that light dark matter may explain a small discrepancy in the measured value of the fine structure constant in different experiments 8 Furthermore the lack of dark matter signals in higher energy ranges in direct detection experiments incentivizes sub GeV searches Theoretical Models for Light Dark Matter editDue to the constraints placed on the mass of WIMPs in the popular freeze out model which predict WIMP masses greater than 2 GeV the freeze out model must be altered to allow for lower mass dark matter particles 9 Scalar Dark Matter edit The Lee Weinberg limit which restricts the mass of dark matter particles to gt 2 GeV may not apply in two special cases where dark matter is a scalar particle 2 The first case requires that the scalar dark matter particle is coupled with a massive fermion This model rules out dark matter particles less than 100 MeV because observations of gamma ray production do not align with theoretical predictions for particles in this mass range This discrepancy may be resolved by requiring an asymmetry between the dark matter particles and antiparticles as well as adding new particles 4 The second case predicts that the scalar dark matter particle is coupled with a new gauge boson The production of gamma rays due to annihilation in this case is predicted to be very low 4 Freeze In Model edit The thermal freeze in model proposes that dark matter particles were very weakly interacting shortly after the Big Bang such that they were essentially decoupled from the plasma Furthermore their initial abundance was small Dark matter production occurs predominantly when the temperature of the plasma falls under the mass of the dark matter particle itself This is in contrast to the thermal freeze out theory in which the initial abundance of dark matter was large and differentiation into lighter particles decreases and eventually stops as the temperature of the plasma decreases 10 The freeze in model allows for dark matter particles well under the 2 GeV mass limit to exist 11 Asymmetric Dark Matter edit Observations show that the density of dark matter is about 5 times the density of baryonic matter Asymmetric dark matter theories attempt to explain this relationship by suggesting that the ratio between the number densities of particles and antiparticles is the same in baryonic matter as it is in dark matter This further implies that the mass of dark matter is close to 5 times the mass of baryonic matter placing the mass of dark matter in the few GeV range 12 Experiments editIn general the methods for detecting dark matter which apply to all heavier dark matter candidates also apply to light dark matter These methods include direct detection and indirect detection Dark matter particles with masses lighter than 1 GeV can be directly detected by searching for electron recoils The greatest difficulty in using this method is creating a detector with a low enough threshold energy for detection while also minimizing background signals Electron beam dump experiments can also be used to search for light dark matter particles 13 XENON10 edit XENON10 is a liquid xenon detector that searches for and places limits on the mass of dark matter by directly detecting electron recoil This experiment placed the first sub GeV limits on the mass of dark matter using direct detection in 2012 14 SENSEI edit SENSEI is a silicon detector capable of measuring the electronic recoil of a dark matter particle between 500 keV and 4 MeV using CCD technology 15 The experiment has been working to place further rule out possible mass ranges of dark matter below 1 GeV with its most recent results being published in October 2020 16 See also editAxion Axion Dark Matter Experiment Dark matter halo Minimal Supersymmetric Standard Model Neutralino Scalar field dark matter Weakly interacting massive particles Weakly interacting slender particlesReferences edit Casse M Fayet P 4 9 July 2005 Light Dark Matter 21st IAP Colloquium Mass Profiles and Shapes of Cosmological Structures Paris arXiv astro ph 0510490 Bibcode 2006EAS 20 201C doi 10 1051 eas 2006072 a b Lee B W Weinberg S 1977 Cosmological Lower Bound on Heavy Neutrino Masses Physical Review Letters 39 4 165 168 Bibcode 1977PhRvL 39 165L doi 10 1103 PhysRevLett 39 165 Bird C Kowalewski R Pospelov M 2006 Dark matter pair production in b s transitions Mod Phys Lett A 21 6 457 478 arXiv hep ph 0601090 Bibcode 2006MPLA 21 457B doi 10 1142 S0217732306019852 S2CID 119072470 a b c Boehm C Fayet P 2004 Scalar Dark Matter candidates Nuclear Physics B 683 1 2 219 263 arXiv hep ph 0305261 Bibcode 2004NuPhB 683 219B doi 10 1016 j nuclphysb 2004 01 015 S2CID 17516917 Boehm C Fayet P Silk J 2004 Light and Heavy Dark Matter Particles Physical Review D 69 10 101302 arXiv hep ph 0311143 Bibcode 2004PhRvD 69j1302B doi 10 1103 PhysRevD 69 101302 S2CID 119465958 Boehm C 2004 Implications of a new light gauge boson for neutrino physics Physical Review D 70 5 055007 arXiv hep ph 0405240 Bibcode 2004PhRvD 70e5007B doi 10 1103 PhysRevD 70 055007 S2CID 41227342 Beacom J F Bell N F Bertone G 2005 Gamma Ray Constraint on Galactic Positron Production by MeV Dark Matter Physical Review Letters 94 17 171301 arXiv astro ph 0409403 Bibcode 2005PhRvL 94q1301B doi 10 1103 PhysRevLett 94 171301 PMID 15904276 S2CID 20043249 Boehm C Ascasibar Y 2004 More evidence in favour of Light Dark Matter particles Physical Review D 70 11 115013 arXiv hep ph 0408213 Bibcode 2004PhRvD 70k5013B doi 10 1103 PhysRevD 70 115013 S2CID 119363575 Roszkowski Leszek Sessolo Enrico Maria Trojanowski Sebastian 2018 05 21 WIMP dark matter candidates and searches current status and future prospects Reports on Progress in Physics 81 6 066201 arXiv 1707 06277 Bibcode 2018RPPh 81f6201R doi 10 1088 1361 6633 aab913 ISSN 0034 4885 PMID 29569575 S2CID 4166809 Hall Lawrence J Jedamzik Karsten March Russell John West Stephen M 2010 Freeze In Production of FIMP Dark Matter PDF Journal of High Energy Physics 2010 3 80 arXiv 0911 1120 Bibcode 2010JHEP 03 080H doi 10 1007 JHEP03 2010 080 S2CID 119166813 via Springer Dvorkin Cora Lin Tongyan Schutz Katelin 2021 09 09 The cosmology of sub MeV dark matter freeze in Physical Review Letters 127 11 111301 arXiv 2011 08186 Bibcode 2021PhRvL 127k1301D doi 10 1103 PhysRevLett 127 111301 ISSN 0031 9007 PMID 34558939 S2CID 226976117 Zurek Kathryn M 2014 04 20 Asymmetric Dark Matter Theories signatures and constraints Physics Reports Asymmetric Dark Matter Theories signatures and constraints 537 3 91 121 arXiv 1308 0338 Bibcode 2014PhR 537 91Z doi 10 1016 j physrep 2013 12 001 ISSN 0370 1573 S2CID 118542568 Diamond Miriam D Schuster Philip 2013 11 27 Searching for Light Dark Matter with the SLAC Millicharge Experiment Physical Review Letters 111 22 221803 arXiv 1307 6861 Bibcode 2013PhRvL 111v1803D doi 10 1103 PhysRevLett 111 221803 ISSN 0031 9007 PMID 24329439 S2CID 7344960 Essig Rouven Manalaysay Aaron Mardon Jeremy Sorensen Peter Volansky Tomer 2012 07 12 First Direct Detection Limits on Sub GeV Dark Matter from XENON10 Physical Review Letters 109 2 021301 arXiv 1206 2644 Bibcode 2012PhRvL 109b1301E doi 10 1103 PhysRevLett 109 021301 ISSN 0031 9007 PMID 23030151 S2CID 14131974 Crisler Michael Essig Rouven Estrada Juan Fernandez Guillermo Tiffenberg Javier Haro Miguel Sofo Volansky Tomer Yu Tien Tien SENSEI Collaboration 2018 08 08 SENSEI First Direct Detection Constraints on Sub GeV Dark Matter from a Surface Run Physical Review Letters 121 6 061803 arXiv 1804 00088 Bibcode 2018PhRvL 121f1803C doi 10 1103 PhysRevLett 121 061803 ISSN 0031 9007 PMID 30141688 S2CID 52077932 Barak Liron Bloch Itay M Cababie Mariano Cancelo Gustavo Chaplinsky Luke Chierchie Fernando Crisler Michael Drlica Wagner Alex Essig Rouven Estrada Juan Etzion Erez 2020 10 20 SENSEI Direct Detection Results on sub GeV Dark Matter from a New Skipper CCD Physical Review Letters 125 17 171802 arXiv 2004 11378 Bibcode 2020PhRvL 125q1802B doi 10 1103 PhysRevLett 125 171802 hdl 11336 138737 ISSN 0031 9007 PMID 33156657 S2CID 216144756 Further reading editBertone Gianfranco 2010 Particle Dark Matter Observations Models and Searches Cambridge University Press p 762 Bibcode 2010pdmo book B ISBN 978 0 521 76368 4 Retrieved from https en wikipedia org w index php title Light dark matter amp oldid 1184875037, wikipedia, wiki, book, books, library,

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