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"BLACK MATTER" what is it? wheres it come from? |
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| Feb21-12, 11:57 AM | #1 |
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"BLACK MATTER" what is it? wheres it come from?
"BLACK MATTER" what is it? wheres it come from?
how is it related to its opposite force the BLACK ENERGY? why is it so powerful? why and why indeed LIGHT wouldn't go through it? put your thoughts here and let's if we can come up with something...... |
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| Feb21-12, 12:01 PM | #2 |
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There is no such thing as black matter or black energy.
Perhaps you mean dark matter and dark energy? |
| Feb21-12, 12:21 PM | #3 |
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i wanted to have a little discussion over here about it if thats not a problem! |
| Feb21-12, 12:26 PM | #4 |
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"BLACK MATTER" what is it? wheres it come from?They are not opposite forces. Dark matter is the name applied to an undetermined type of matter that seems to be affected by gravity but does not seem to interact with normal matter or light at all. Dark energy is a term applied to whatever is causing the expansion of the universe. |
| Feb21-12, 12:38 PM | #5 |
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and the dark matter basically make stuff stick together is that right?
galaxies would stay stiff by dark M and the universe being made of galaxies is expanding caused by dark E.. why is that? im sorry if i ask basic question im new to cosmology |
| Feb21-12, 02:29 PM | #6 |
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That's basically the correct distinction. Dark matter gravitates like ordinary visible matter, but it doesn't interact electromagnetically so it's effectively pressureless. This means that it easily clumps and plays an important role in the formation of gravitationally bound structures like galaxies.
As for dark energy, it gravitates differently. It is assumed to be smoothly distributed throughout the universe, not clumping like dark matter. Its gravitational behavior instead results in an accelerated expansion. Though not directly detected, dark matter is supported by a variety of observations, including evidence from structure formation, the cosmic microwave background, and gravitational lensing. Dark energy, as DaveC mentions, is rather speculative; it's the name we give to the hypothetical source driving the expansion. |
| Feb21-12, 02:54 PM | #7 |
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wow thanks
so heres the part i dont really get .. how it doesnt interact electromagnetically? based on that its not following the rules of physics as other matters would do. because even energy cannot go through it, it should be intact am i right? then can we trace its root? |
| Feb21-12, 03:57 PM | #8 |
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| Feb21-12, 05:48 PM | #9 |
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| Feb22-12, 05:21 AM | #10 |
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now im thinking of something ... this universe is full of exact particles that are found in atoms dark matter explains the neutron(sort of) and electrons are energy and protons generate gravity; if we put it this way this universe is actually an atom ! .... let me get back to dark energy.. isn't it just the "time" ? it is clearly causing us move forward. galaxies, clusters, super clusters are going somewhere in all directions, they are spending time due to the dark energy, make sense? |
| Feb22-12, 07:45 AM | #11 |
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| Feb22-12, 08:04 AM | #12 |
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Dark matter does not consist of neutrons, and there are not nearly enough neutrinos to account for all the missing mass in the universe [at least not any species currently known to science]. Neutrinos do, however, behave very much like dark matter in that they barely interact with other forms of matter. The big difference appears to be mass. There are three 'flavors' of neutrinos we currently know of and their mass is somewhere in the rage of .05 - .28 electron volts. The electron is a mountain by comparison at 931 MILLION electron volts. A more massive version of the neutron [e.g., WIMP] would be a perfect dark matter candidate. Neutrinos are enormously abundant in the universe, almost as numerous as CMB photons. If dark matter particles are similarly abundant, their mass need not be more than a few electron volts - still little more than a gnat compared to the 800 lb gorilla we call the electron.
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| Feb22-12, 08:38 AM | #13 |
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| Feb22-12, 09:52 AM | #14 |
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I believe he is making a comparison:
dark matter is to neutrons as energy is to electrons and gravity is to protons (whether this is a valid comparison at all is something I won't comment on) and not trying to state what comprises dark matter. |
| Feb27-12, 06:52 AM | #15 |
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| Mar1-12, 05:49 AM | #16 |
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Lai, Xiao-Yu of Peking University proposed that " Strange quark nuggets (SQNs) could be the relics of the cosmological QCD phase transition, and they could very likely be the candidate of cold dark matter if survived the cooling of the later Universe, although the formation and evolution of these SQNs depend on the physical state of the hot QGP (quark-gluon plasma) phase and the state of cold quark matter. We reconsider the possibility of SQNs as cold dark matter, and discuss the astrophysical consequences of primordial SQNs in the early and present universe. In the early Universe, the formation of black holes inside primordial halos could be faster than that in the standard scenario, and speed up the formation of the supermassive black holes at high redshift. In the present Universe, the capture of SQNs by pulsars could trigger star-quakes, which could be the mechanism for pulsar-glitches." - 1st Caribbean Symposium on Cosmology, Gravitation, Nuclear and Astroparticle Physics: STARS2011
1-4 May 2011: La Habana, Cuba where as Tomohiro Abe, Mitsuru Kakizaki, Shigeki Matsumoto, Osamu Seto. proposed that "Weakly interacting massive particle (WIMP) is well known to be a good candidate for dark matter, and it is also predicted by many new physics models beyond the standard model at the TeV scale. We found that, if the WIMP is a vector particle (spin one particle) which is associated with some gauge symmetry broken at the TeV scale, the higgs mass is often predicted to be 120--125 GeV, which is very consistent with the result of higgs searches recently reported by ATLAS and CMS collaborations at the Large Hadron Collider experiment. In this letter, we consider the vector WIMP using a non-linear sigma model in order to confirm this result as general as possible in a bottom-up approach. Near-future prospects to detect the vector WIMP at both direct and indirect detection experiments of dark matter are also discussed.-UT-HET-063,IPMU12-0029,HGU-CAP-14 e-Print: arXiv:1202.5902 [hep-ph] Reference : Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Interpretation - WMAP Collaboration (Komatsu, E. et al.) Astrophys.J.Suppl. 192 (2011) 18 . arXiv:1001.4538 [astro-ph.CO] Bounds on universal extra dimensions - Appelquist, Thomas et al. Phys.Rev. D64 (2001) 035002 . hep-ph/0012100 . hep-ph/0012100,YCTP-P12-00,EFI-2000-48 Dark matter and collider phenomenology of universal extra dimensions - Hooper, Dan et al. Phys.Rept. 453 (2007) 29-115 . hep-ph/0701197 . hep-ph/0701197,FERMILAB-PUB-07-018-A Electroweak symmetry breaking from dimensional deconstruction - Arkani-Hamed, Nima et al. Phys.Lett. B513 (2001) 232-240 . hep-ph/0105239 . hep-ph/0105239,HUTP-01-A024,BUHEP-01-06,UCB-PTH-01-15 The Minimal moose for a little Higgs - Arkani-Hamed, N. et al. JHEP 0208 (2002) 021 . hep-ph/0206020 . hep-ph/0206020,BUHEP-02-24,UW-PT-01-09,HUTP-02-A016 TeV symmetry and the little hierarchy problem - Cheng, Hsin-Chia et al. JHEP 0309 (2003) 051 . hep-ph/0308199 . hep-ph/0308199,HUTP-03-A051 Little hierarchy, little Higgses, and a little symmetry - Cheng, Hsin-Chia et al. JHEP 0408 (2004) 061 . hep-ph/0405243 . hep-ph/0405243 Little Higgs models and their phenomenology - Perelstein, Maxim Prog.Part.Nucl.Phys. 58 (2007) 247-291 . hep-ph/0512128 . hep-ph/0512128 Combined search for the Standard Model Higgs boson using up to 4.9 fb-1 of pp collision data at sqrt(s) = 7 TeV with the ATLAS detector at the LHC - ATLAS Collaboration . arXiv:1202.1408 [hep-ex] . CERN-PH-EP-2012-019 Combined results of searches for the standard model Higgs boson in pp collisions at sqrt(s) = 7 TeV - CMS Collaboration (Chatrchyan, Serguei et al.) . arXiv:1202.1488 [hep-ex] . CMS-HIG-11-032,CERN-PH-EP-2012-023 A Tool Kit For Builders Of Composite Models - Georgi, Howard Nucl.Phys. B266 (1986) 274 . HUTP-85/A060 Cosmic abundances of stable particles: Improved analysis - Gondolo, Paolo et al. Nucl.Phys. B360 (1991) 145-179 . UCLA-90-TEP-68 MicrOMEGAs 2.0: A Program to calculate the relic density of dark matter in a generic model - Belanger, G. et al. Comput.Phys.Commun. 176 (2007) 367-382 . hep-ph/0607059 . hep-ph/0607059,LAPTH-1152-06 Indirect search for dark matter with micrOMEGAs2.4 - Belanger, G. et al. Comput.Phys.Commun. 182 (2011) 842-856 . arXiv:1004.1092 [hep-ph] . IRFU-10-24,LAPTH-012-10. LanHEP - a package for automatic generation of Feynman rules from the Lagrangian. Updated version 3.1 - Semenov, A. . arXiv:1005.1909 [hep-ph] Supersymmetric dark matter - Jungman, Gerard et al. Phys.Rept. 267 (1996) 195-373 . hep-ph/9506380 . hep-ph/9506380,SU-4240-605,UCSD-PTH-95-02,IASSNS-HEP-95-14,CU-TP-677 Direct Detection of Vector Dark Matter - Hisano, Junji et al. Prog.Theor.Phys. 126 (2011) 435-456 . arXiv:1012.5455 [hep-ph] . IPMU10-0227,CALT-68-2815,MISC-2010-20 Nucleon strange quark content from two-flavor lattice QCD with exact chiral symmetry - JLQCD Collaboration (Takeda, K. et al.) Phys.Rev. D83 (2011) 114506 . arXiv:1011.1964 [hep-lat] . UTHEP-615,KEK-CP-241 Dark Matter Results from 100 Live Days of XENON100 Data - XENON100 Collaboration (Aprile, E. et al.) Phys.Rev.Lett. 107 (2011) 131302 . arXiv:1104.2549 [astro-ph.CO] First results of XENON100 - XENON100 Collaboration (Schumann, Marc for the collaboration) PoS IDM2010 (2011) 029 Constraining Dark Matter Models from a Combined Analysis of Milky Way Satellites with the Fermi Large Area Telescope - Fermi-LAT Collaboration (Ackermann, M. et al.) Phys.Rev.Lett. 107 (2011) 241302 . arXiv:1108.3546 [astro-ph.HE] PAMELA results on the cosmic-ray antiproton flux from 60 MeV to 180 GeV in kinetic energy - PAMELA Collaboration (Adriani, O. et al.) Phys.Rev.Lett. 105 (2010) 121101 . arXiv:1007.0821 [astro-ph.HE] Antiprotons from dark matter annihilation in the Galaxy: astrophysical uncertainties - Evoli, Carmelo et al. . arXiv:1108.0664 [astro-ph.HE] . DESY-11-135 Is the lightest Kaluza-Klein particle a viable dark matter candidate? - Servant, Geraldine et al. Nucl.Phys. B650 (2003) 391-419 . hep-ph/0206071 . hep-ph/0206071,ANL-HEP-PR-02-032,EFI-02-74 Significant effects of second KK particles on LKP dark matter physics - Kakizaki, Mitsuru et al. Phys.Rev. D71 (2005) 123522 . hep-ph/0502059 . hep-ph/0502059,ICRR-514-2004-12,STUPP-05-178 JCAP,1102,009 I have cited the latest of the 2 from http://inspirehep.net/search?ln=en&l...m=&rg=100&sc=1 I like this website for uptodate High Energy Physics (HEP) information system. |
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