Non-baryonic dark matter

DAMA/NaI + mirror matter

Dark Matter Detection - DAMA/NaI + Foot et al.

• In http://de.arxiv.org/abs/astro-ph/0405282 the 7 year results of the DAMA/NaI dark matter direct detection experiment show a signal significant at 6.3σ according to the authors. An explanation for why a signal from mirror-baryonic matter should be expected in this experiment but not in others with similar cross-section detection parameters is presented in AstroPh:0403043, see also AstroPh:0407623 and references therein.
• Aim: Check the experimental and theoretical claims and propose further tests
  • Try to find an alternative explanation for the DAMA/NaI results without going beyond the Standard Model of particle physics
  • Check whether the Foot et al. calculations of mirror matter properties are consistent with all the experimental data as the authors claim
  • Extend the Foot et al. calculations to find, e.g. a non-gravitational effect of mirror matter in stellar physics, e.g. symbiotic stars (gravitational effects of dark matter are already well studied)
• More info: http://adjani.astro.uni.torun.pl/Cosmo/NonBaryonicDarkMatter#the_DAMA_NaI_detection_and_mirro

the DAMA/NaI detection and mirror matter: longer introduction

• AstroPh:0305542 - see Fig.~6 - mass: m_W~43⁺¹²_-9GeV (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
    • 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_min=1560km/s. This is also too high.
    • For Na + He' + 1keV, v_min=310km/s - this is much more consistent with the halo temperature.
    • For Ge + O' + 10keV, v_min=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: mirrorvelocity.f
• mirror matter claims independent of DAMA
  • AstroPh:0211067 - mirror matter from Eros lower limit to crater size
  • HepPh:0402267 - Ω_b=0.2Ω_DM 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

Dark Matter - Light Dark Matter (LDM) hypothesis - Galaxy Centre INTEGRAL results

• http://arxiv.org/abs/astro-ph/0507142
• Is the 511 keV line emission in the galactic centre due to annihilating LDM?

Review/Introduction papers on Non-Baryonic Dark Matter problem

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

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
  • 
    • where , directly depends on c with no free parameters
    • values of c range from about 5-20 (see p563), i.e. 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 cosmological calculator)
• Equation of state for different components of the Universe (i.e. nbCDM) and it's influence on cosmological parameters evolution