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%TOC% Zobacz też: NonBaryonicDarkMatterPl (wersja polska) ---- ---+ Non-baryonic dark matter ---++ DAMA/NaI + mirror matter _źródło: DAMAStudentTematAbstrakt_ %INCLUDE{"DAMAStudentTematAbstrakt"}% ---+++ the DAMA/NaI detection and mirror matter: longer introduction * AstroPh:0305542 - see Fig.~6 - mass: m<sub>W</sub>~43<sup>+12</sup><sub>-9</suB>GeV (for v = 220km/s) - Bernabei et al - but mass depends strongly on halo model - see also AstroPh:0304446 * (eV conversion: WikipediaPl:Elektronowolt, Wikipedia:Electronvolt) * CosmoNews * DAMA * AstroPh:0405282 - 7 yr DAMA/NaI data * HepPh:0308254, AstroPh:0403043 - mirror matter to explain DAMA data * HepPh:0210370 - parameter space of cross-section and WIMP mass excluded by other experiments (DAMA/Xe, Edelweiss). However, this is only valid for a certain class of interaction. It is invalid for mirror matter WIMPs. * in HepPh:0308254, Foot points out that for a direct detection experiment like DAMA/Xe or Edelweiss to succeed, the required velocity of the particles must not be too much higher than typical velocities in the halo. This maximum velocity - eq. (5) is %$ v_{\mbox{min}} = \sqrt{ { (M_A + M_{A'})^2 E_R \over 2 M_A M_{A'}^2 } } $% * For either Germanium (Edelweiss, CDMS, ...) or Na interacting with H' (mirror H) and a threshold of 4-10keV, the minimum velocity is about 2200km/s. This is only the very tail end of any realistic galactic velocity distribution. * For Ge + He' + 10keV, v<sub>min</sub>=1560km/s. This is also too high. * For Na + He' + 1keV, v<sub>min</sub>=310km/s - this is *much* more consistent with the halo temperature. * For Ge + O' + 10keV, v<sub>min</sub>=450km/s. So, if there is a *big* O' component - mirror O in the halo, then Edelweiss probably should have detected it. However, in HepPh:0308254 the claim is for a He' dominant component (with H' undetectable) and only a minor O' component. * A short fortran script to calculate these is here: [[%ATTACHURL%/mirrorvelocity.f][mirrorvelocity.f]] * mirror matter claims independent of DAMA * AstroPh:0211067 - mirror matter from Eros lower limit to crater size * HepPh:0402267 - Ω<sub>b</sub>=0.2Ω<sub>DM</sub> where DM = mirror-baryonic matter * prezentacja pdf - pażd 2004 - http://cosmo.torun.pl/~boud/wyklad041025.pdf * wikipedia discussion page: WikipediaEn:Talk:Mirror_matter ---++ Light Dark Matter - the INTEGRAL results _źródło: LDMStudentTematAbstrakt_ %INCLUDE{"LDMStudentTematAbstrakt"}% ---++ Review/Introduction papers on Non-Baryonic Dark Matter problem big-bang nucleosynthesis (BBN), e.g. Steigmann AstroPh:0511534 %$\Rightarrow \Omega_{nonbaryonic} \sim 0.25$% ---+++ WIMPS (and other new particles) * AstroPh:0402045 Martin Rees - recent, quick and short * AstroPh:0506676 pages 5,6,7 Paul Frampton - recent, quantified, quick, short summary * AstroPh:0403064 Paul Gondolo - recent, *in-depth* introduction * AstroPh:0511805 Laura Baudis - listopad 2005r. ---+++ MACHOS * recent MACHO articles: http://arxiv.org/find/astro-ph/1/ti:+machos/0/1/0/all/0/1 * MACHO debate: are the MW microlensing events only due to known stellar populations? * Evans & Belokurov, 2004, RIP: The Macho Era (1974-2004) AstroPh:0411222 vs * Griest & Thomas 2004 Contamination in the MACHO dataset and the puzzle of LMC Microlensing AstroPh:0412443 ---+++ brown dwarfs * brown dwarfs are baryonic: they cannot explain %$\Rightarrow \Omega_{nonbaryonic} \sim 0.25$% ---+++ pierwotny czarny dziury - primordial black holes * Afshordi et al. AstroPh:0302035 Primordial Black Holes as Dark Matter: The Power Spectrum and Evaporation of Early Structures ---++ nBDM density profile in Milky Way * joe silk paper - http://www.astro.uni.torun.pl/sympa/cosmo-torun/2004-01/msg00000.html * DM profile < 50kpc, < 100kpc, up to few 100kpc http://www.astro.uni.torun.pl/sympa/cosmo-torun/2004-01/msg00003.html * AstroPh:0401140 - neutralino annihilation - is this the same as SIDM (self-interacting dark matter?) * AstroPh:0307026 - _Dark matter annihilation in the halo of the Milky Way_ - Felix Stoehr, Simon D. M. White, Volker Springel, Giuseppe Tormen, Naoki Yoshida * AstroPh:0401575 - _scalar field ,,toy" model of SIDM matches observations_ Fuchs, Mielke * classic Navarro, Frenk & White paper (1996): http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1996ApJ...462..563N * %$ {\delta(r) \over \delta_{\mbox{\tiny crit}}} = {\delta_c \over (r/r_s) (1+ r/r_s)^2}} $% * where %$ r_s = r_{200}/c $%, %$ \delta_c $% directly depends on _c_ with no free parameters * values of _c_ range from about 5-20 (see p563), i.e. %$ r_s $% ranges from about 20% (for big haloes) to 5% (for small haloes) of the virial radius - NFR1996 is now very old, but the problem is still probably that of the *inner few kpc* * w<-1.0 seems to help: AstroPh:0402210 Dark Energy and Dark Matter Halos - M. Kuhlen, L.E. Strigari, A.R. Zentner, J.S. Bullock, Joel R. Primack ---++ see also * see also CosmoNews ---++ possible outline of extensive Literature Review * original version by Bartek Lew: http://adjani.astro.uni.torun.pl/~blew/praca/phd/index.html ---+++ primary objectives * Observational possibilities of either direct or indirect detection of cold nonbaryonic dark matter (nbCDM) in the Universe * Research for composition, nature and physics of nbCDM in terms of currently favored candidates (WIMP's, Axions, super heavy relicts). * Galaxy distribution, dynamics, scattering rates and energy deposit in possible interactions of nbCDM for various candidates * Possible observational constraints on nature of nbCDM * Possible connection (interaction) between nbCDM and dark energy (DE) * Current / future possibilities of relevant nbCDM experiments * Some knowledge of standard particle physics and supersymmetric extensions of standard model (MSSM) * (Super)Symmetry breaking problems in cosmology and particle physics ---+++ secondary objectives * Friedmann equations solutions for various cosmological models (see [[http://adjani.astro.uni.torun.pl/~blew/praca/calc/index_en.html][cosmological calculator]]) * Equation of state for different components of the Universe (i.e. nbCDM) and it's influence on cosmological parameters evolution
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Topic revision: r15 - 24 Apr 2006,
BoudRoukema
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