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\sigma_\nu well-known for relic density \sim 10^{-26} cm^3/s
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BBN: 1MeV < m_N
ToK Warszawa meeting - Rough Notes Thu 15 Feb 2007
These are just rough notes - feel free to correct them, add links, etc.Hector Rubinstein - stockholm - magnetic fields
Magnetic fields on kpc scales exist. They may exist on intergalactic scales - it's unclear whether or not their origin is primordial. CMB - Planck - may be able to detect magnetic fields present at the epochs not long after nucleosynthesis and recombination it is well known that photon has a thermal mass - about 10^{-39} [units =eV?] which is extremely small - related to electron loops Maxwell eqns -> Proca eqns WikipediaEn:Proca_action m_photon < 10^-26 eV \exists galactic mag fields at z \approx 3 making dynamo mechanisms difficult to explain themBoehm - LDM hypothesis
511 keV detection
Leventhal(sp?) 199x ApJ OSSE 3 components Purcell et al 1997candidates
stars - SNe, SNII, WR compact sources - pulsars, BH, low mass binaries - most excluded because they would imply 511keV from the disk - SNIa - need large escape fraction and explosion rate to maintain a steady flux - low mass X-ray binaries - need electrons to escape from the disk to the bulgeMeV scale
dm + dm -> e^- + e^+ e+ loses energy -> positronium e+e- -> positronium decays para-positronium 2 gamma - monochromatic wih 511keV ortho-positronium 3 gamma - continuumpredictions
positron emission should be maximal with highest DM concentration (n^2 effect?)cdm spectrum
does NOT produce CDM-like power spectrum??? - at 10^9 M_sun essentially CDM-like - by 10^6 M_sun, the difference would be importantspectrum
Ascasibar et al 2005, 2006model
- through F- 511keV
- through Z' relic density
link with neutrino mass
interaction/decay diagrams -> link between neutrino mass and DM cross section:
\sigma_\nu well-known for relic density \sim 10^{-26} cm^3/s
low energy Beyond SM
MeV DM has definitely escaped all previous low energy experiments due to lack of luminosity BABAR/BES II ... ?summary
...- explains low value of neutrino masses
- detection at LHC may be possible but requires work
- back to SUSY -> snu-neutralino-nu ?
Conlon - hierarchy problems in string theory: the power of large volume
planck scale 10^18 GeV ... cosm constant scale (10^-3eV)^4 - large-volume models can generate hierarchies thorugh a stabilised exponentially large volume - predicts cosmological constant (but about 50 orders of magnitude too large - solving this problem is left to the reader/audience)G\"unther Stigl - high-energy c-rays, gamma-rays, neutrinos
HESS - correlation of observations at GC with molecular cloud distribution KASCADE - has made observations Southern Auger - 1500km^2 - in Chile/Argentina Hillas plot c-rays at highest energies could be protons, could be ions - most interactions produce pions; pi^\pm decays to neutrinos pi^0 decays to photons (gamma-rays)- origin of very high energy c rays remains one of the fundamental unsolved questions of astroparticle physics - even galactic c ray origin is unclear
- acceleration and sky distribution of c rays are strongly linked to the strength and distribution of cosmic magnetic fields - which are poorly known
- sources probably lie in fields of \mu-Gauss
- HE c-rays, pion-production, gamma-ray/neutrinos - all three fields should be considered together; strong constraints arise from gamma-ray overproduction
Khalil - DM - SUSY - brane cosmology
(British University in Egypt = BUE) - friedmann eqn modified in 5D (brane model) - dark matter relic abundanceError during latex2img:
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\begin{math}\displaystyle m_\nu = \sqrt{ \sigma \nu \over 128 \pi^3 } m_N^2 ln{ \Lambd^2/m_N^2 }\end{math}
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l.17 ...ma \nu \over 128 \pi^3 } m_N^2 ln{ \Lambd
^2/m_N^2 }\end{math}
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(see the transcript file for additional information)
Output written on MaXucvm_1V.dvi (1 page, 784 bytes).
Transcript written on MaXucvm_1V.log.
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