2,399 research outputs found
Signatures of the Milky Way's Dark Disk in Current and Future Experiments
In hierarchical structure formation models of disk galaxies, a dark matter
disk forms as massive satellites are preferentially dragged into the disk-plane
where they dissolve. Here, we quantify the importance of this dark disk for
direct and indirect dark matter detection. The low velocity of the dark disk
with respect to the Earth enhances detection rates in direct detection
experiments at low recoil energy. For WIMP masses M_{WIMP} >~ 50 GeV, the
detection rate increases by up to a factor of 3 in the 5 - 20 keV recoil energy
range. Comparing this with rates at higher energy is sensitive to M_{WIMP},
providing stronger mass constraints particularly for M_{WIMP}>~100 GeV. The
annual modulation signal is significantly boosted by the dark disk and the
modulation phase is shifted by ~3 weeks relative to the dark halo. The
variation of the observed phase with recoil energy determines M_{WIMP}, once
the dark disk properties are fixed by future astronomical surveys. The low
velocity of the particles in the dark disk with respect to the solar system
significantly enhances the capture rate of WIMPs in the Sun, leading to an
increased flux of neutrinos from the Sun which could be detected in current and
future neutrino telescopes. The dark disk contribution to the muon flux from
neutrino back conversion at the Earth is increased by a factor of ~5 compared
to the SHM, for rho_d/rho_h=0.5.Comment: 5 pages, 7 figures, To appear in the proceedings of Identification of
Dark Matter 2008 (IDM2008), Stockholm, 18-22 August 2008; corrected one
referenc
Minimal Flavor Violation and the Scale of Supersymmetry Breaking
In this paper we explore the constraints from B-physics observables in SUSY
models of Minimal Flavor Violation, in the large tan beta regime, for both low
and high scale supersymmetry breaking scenarios. We find that the rare B-decays
b -> s gamma and B_s -> mu+ mu- can be quite sensitive to the scale M at which
supersymmetry breaking is communicated to the visible sector. In the case of
high scale supersymmetry breaking, we show that the additional gluino
contribution to the b -> s gamma and B_s -> mu+ mu- rare decay rates can be
significant for large tan beta, mu and M_3. The constraints on B_u -> tau nu
are relatively insensitive to the precise scale of M. We also consider the
additional constraints from the present direct Higgs searches at the Tevatron
in the inclusive H/A -> tau tau channel, and the latest CDMS direct dark matter
detection experiments. We find that altogether the constraints from B-physics,
Higgs physics and direct dark matter searches can be extremely powerful in
probing regions of SUSY parameter space for low M_A and large tan beta, leading
to a preference for models with a lightest CP-even Higgs mass close to the
current experimental limit. We find interesting regions of parameter space that
satisfy all constraints and can be probed by Higgs searches at the Tevatron and
the LHC and by direct dark matter searches in the near future.Comment: 24 pages, 6 figures. Added citations. Published in PR
Changes in HBCU Financial Aid and Student Enrollment After the Tightening of PLUS Credit Standards
We analyze changes in financial aid and student enrollment at historically Black colleges and universities (HBCUs) that occurred after the U.S. Department of Education increased the credit history requirements necessary to obtain Parent Loans for Undergraduate Students (PLUS). We use institution-level data to examine financial aid and enrollment changes in the first two academic years affected by the new credit standards (2012-13 and 2013-14). The results show that PLUS loans declined substantially at HBCUs in 2012-13, and the decreases were not fully replaced by other types of federal financial aid. HBCUs also experienced larger declines in enrollment than other institutions – particularly for first-year students. Though PLUS loans increased somewhat in 2013-14 after the U.S. Department of Education streamlined the appeals process for PLUS denials, enrollment at HBCUs continued to decline
Spectroscopy of Nine Cataclysmic Variable Stars
We present optical spectroscopy of nine cataclysmic binary stars, mostly
dwarf novae, obtained primarily to determine orbital periods Porb. The stars
and their periods are LX And, 0.1509743(5) d; CZ Aql, 0.2005(6) d; LU Cam,
0.1499686(4) d; GZ Cnc, 0.0881(4) d; V632 Cyg, 0.06377(8) d; V1006 Cyg,
0.09903(9) d; BF Eri, 0.2708804(4) d; BI Ori, 0.1915(5) d; and FO Per, for
which Porb is either 0.1467(4) or 0.1719(5) d.
Several of the stars proved to be especially interesting. In BF Eri, we
detect the absorption spectrum of a secondary star of spectral type K3 +- 1
subclass, which leads to a distance estimate of approximately 1 kpc. However,
BF Eri has a large proper motion (100 mas/yr), and we have a preliminary
parallax measurement that confirms the large proper motion and yields only an
upper limit for the parallax. BF Eri's space velocity is evidently large, and
it appears to belong to the halo population. In CZ Aql, the emission lines have
strong wings that move with large velocity amplitude, suggesting a
magnetically-channeled accretion flow. The orbital period of V1006 Cyg places
it squarely within the 2- to 3-hour "gap" in the distribution of cataclysmic
binary orbital periods.Comment: 31 pages, 5 postscript and one PNG figure. Accepted for PAS
Emission Line Flickering from the Secondary Star in Cataclysmic Variables? A study of V3885 Sagitarii
Spectrophotometric observations of H-alpha and He I 6678 emission lines of
the nova-like Cataclysmic Variable V3885 Sgr are presented and analyzed. The
binary orbital period was determined as P = 0.20716071(22) days. Doppler
Tomography was performed with both H-alpha and He I lines. Disc radial
emissivity profiles were also computed. The tomography mapping of flickering
sources was performed using the H-alpha line, from which we concluded that the
flickering is not uniformly distributed on the disc. The observed tomogram of
the flickering was compared with simulations, suggesting that the most intense
flickering source in the H-alpha is not located in the accretion disc. It is
proposed that the main line flickering source may be associated with the
illuminated secondary star.Comment: 19 pages, 10 figures, 1 table. Accepted to be published on AJ. to
donwload high resolution figures:
http://www.astro.iag.usp.br/~fabiola/V3885_hires.pd
FUSE Observations of the Dwarf Novae UU Aql, BV Cen, and CH UMa in Quiescence
We report on FUSE spectra of three U Gem-type, long period, dwarf novae, UU
Aql, BV Cen and CH UMa taken during their quiescence intervals. We discuss the
line identifications in their spectra and attempt to characterize the source(s)
of their FUV flux distribution. Archival IUE spectrum of CH UMa and BV Cen in
quiescence were identified as having a matching flux level with the FUSE
spectra and these were combined with each FUSE spectrum to broaden the
wavelength coverage and further constrain model fits. Multi-component synthetic
spectral fits from our model grids, consisting of single temperature white
dwarfs, two-temperature white dwarfs, accretion disks and white dwarfs plus
accretion disks, were applied to the FUSE spectra alone and to the combined
FUSE + IUE spectra. We present the results of our model analyses and their
implications.Comment: accepted in AJ, 26 pages, 6 tables, 8 figures (5 color, 3 b/w
Reconstructing palaeotemperatures using leaf floras – case studies for a comparison of leaf margin analysis and the coexistence approach
AbstractIn the past the problems and advantages of the nearest-living-relative (NLR) and leaf physiognomy approaches have been repeatedly discussed and it has been demonstrated that both approaches frequently show broad agreement with each other. However, detailed comparisons of the various methods for accuracy in estimation of palaeoclimate at individual localities are still lacking. Such studies are needed before data obtained from different approaches can be integrated in palaeoclimate maps and models. Moreover, there are some indications that leaf physiognomy and NLR approaches may lead to different results. In this study we applied a physiognomic method based on leaf margin analysis and the coexistence approach, a recent variation of the NLR approach, to two Tertiary palaeofloras (Schrotzburg, Middle Miocene, south Germany; Kleinsaubernitz, Upper Oligocene, east Germany). We demonstrated that both approaches can produce reasonable and consistent results if the standard error of the leaf physiognomy palaeoclimate data is taken into account. However, our results and interpretations indicate that reconstructions based on leaf physiognomy are influenced by factors not related to climate, such as sample size and differential preservation or transport. In contrast, reconstructions for the same fossil assemblages based on the coexistence approach seem to be less affected by taphonomic variables, but may be less sensitive to minor climate changes
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