Thursday---already. I worked all day yesterday. Caught a cold, just like dad. I'm still a full week behind on Astro-ph! I'm also getting used to using the dishwasher--not sure if that's a good sign.
1112.3771
Outer disks of lentitular galaxies
Silchenko
Study stellar population properties along the radius in 15 nearby S0s: find outer stellar disks are old (8-15 Gyr), being often older than bulges. S0 formation theory (quenched SF in spiral galaxies) questioned.
1112.3809
Modeling the spectra of (BAL) QSOs
Higginbottom, Long, Knigge, Sim
Model QSO spectra, investigate the plausibility of geometric unification. For reasonable geometries and mass loss rates, able to produce synthetic spectra which reproduce the features of BALQSO spectra.
1112.3824
Chemical evolution of the MW: the origin of phosphorus
Cescutti, Matteucci, Caffau, Francois
Abundance of P measured in disk stars. Predict chemical evolution of P in MW and compare results with observation to put constraints on the P nucleosynthesis. Adopt two-infall model [?], compute the evolution of abundances of P and Fe. Adopt stellar yields for these elements from different sources. P should have been formed mainly in Type II SNe. Fe mainly in Ia SNe. Results: confirm that, to reproduce the observed trend of [P/Fe] vs [Fe/H] in disk stars, P is formed mainly in massive stars. But in order to reproduce the data, the massive stars should produce x3 more P than predicted. Conclude: available yields from P from massive stars are largely underestimated, nucleosynthesis calculations should be revised. Predict [P/Fe] expected in halo stars.
1112.3860
Detection of HF emission from the Orion Bar
van der Tak, Ossenkopf, Nagy, Faure, Roellig, Bergin
Conclude that HF emission is a signpost of molecular gas with high electron density.
* HF line signpost of molecular gas + high electron density (plasma).
* HF line signpost of molecular gas + high electron density (plasma).
1112.3875
The cenetral PNe populations of external galaxies with SAURON
Sarzi
PNe in M32 and M31: lack of bright PNe in the nuclear regions of M31 is likely linked to the nearly Solar value for the stellar metallicity, consistent with suggestions that a larger metallicity would bias the horizontal-branch (HB) populations toward bluer colors, with fewer red HB stars capable of producing PNe and more HB stars contribute to the far UV that is observed in metal-rich early-type galaxies, as well as in the nucleus of M31.
* blue HB stars generate far UV radiation.
1112.3889
Fullerenes and proto-fullerenes in interstellar carbon dust
Duley, Hu
What was thought to be C60 emission lines are actually from precursor molecules in hydrogenated amorphous carbon (HAC).
1112.3893
The X-ray properties of Cataclysmic variables
Balman
Cataclysmic variables (CVs) are a distinct class of X-ray binaries transferring mass from a donor star to a compact star accretor (WD). A lab for accretion physics, mechanisms and disk theory with dynamics of outflows and interaction with surrounding medium. More data on accretion shocks and boundary layers with high sensitivity instruments and/or grating X-ray spectroscopy with high resolution, yielding temperature and velocity diagnostics. Time resolution utilizes accretion mode diagnostics, characterizing the variability of the gas flow in disks. Review Intermediate Polars, Dwarf Novae and Classical/Recurrent Novae.
1112.3895
Constructing regularized cosmic propagators
Bernardeau, Crocce, Scoccimarro
New scheme for general computation of cosmic propagators that allow interpolation between standard perturbative results at low-k and their expected large-k resummed behavior. [what is a propagator?] Generic prescription for multi-point propagators provides the necessary building blocks for computation of polyspectra in the context of "Gamma-expansion" (by Bernardeau+ 08). Apply to calculation of the matter bispectrum at one-loop order.
1112.3897
Inflationary magnetic fields spoil the homogeneity and isotropy of the Universe
Bonvin, Caprini, Durrer
As the title says.
1112.3901
1112.3889
Fullerenes and proto-fullerenes in interstellar carbon dust
Duley, Hu
What was thought to be C60 emission lines are actually from precursor molecules in hydrogenated amorphous carbon (HAC).
1112.3893
The X-ray properties of Cataclysmic variables
Balman
Cataclysmic variables (CVs) are a distinct class of X-ray binaries transferring mass from a donor star to a compact star accretor (WD). A lab for accretion physics, mechanisms and disk theory with dynamics of outflows and interaction with surrounding medium. More data on accretion shocks and boundary layers with high sensitivity instruments and/or grating X-ray spectroscopy with high resolution, yielding temperature and velocity diagnostics. Time resolution utilizes accretion mode diagnostics, characterizing the variability of the gas flow in disks. Review Intermediate Polars, Dwarf Novae and Classical/Recurrent Novae.
1112.3895
Constructing regularized cosmic propagators
Bernardeau, Crocce, Scoccimarro
New scheme for general computation of cosmic propagators that allow interpolation between standard perturbative results at low-k and their expected large-k resummed behavior. [what is a propagator?] Generic prescription for multi-point propagators provides the necessary building blocks for computation of polyspectra in the context of "Gamma-expansion" (by Bernardeau+ 08). Apply to calculation of the matter bispectrum at one-loop order.
1112.3897
Inflationary magnetic fields spoil the homogeneity and isotropy of the Universe
Bonvin, Caprini, Durrer
As the title says.
1112.3901
Magnetic fields from inflation: the fatal transition to the radiation era
Bonvin, Caprini, Durrer
Same as above.
1112.3903
An estimate of the temporal fraction of cloud cover at San Pedro M'artier Observatory
Carasco, Carraminana, Sanchez, Avila, Cruz-Gonzalez
Find 82.4 % of the time the sky is clear of clouds at this site.
1112.3911
Galactic sources of high-energy neutrinos: Highlights
Vissani, Aharonian
Overview of high-energy neutrinos from galactic sources, transparent [?] to their gamma-ray emission [?]. Focus on young SNe remnants. Consider possibility of detecting neutrinos from other strong galactic gamma-ray sources, such as Vela Junior, Cygnus Region and Fermi Bubbles. Quantify the impact of large theta_13 on high-energy neutrino oscillations.
1112.3917
Detection of very high energy gamma-ray emission from NGC 1275 by the MAGIC telescopes
MAGIC collaboration, Lombardi, Colin, Hildebrand, Zandanel
VHE gamma-ray emission (E>100 GeV) from NGC 1275, the central radio galaxy of the Perseus cluster of galaxies. Fermi-LAT measured spectra above 100 MeV. Indicates a break or cut-off around ~10s GeV in the spectrum. E > 100 GeV does not show variability in the month timescale. Non-detection of radio galaxy IC 310. VHE has a variability timescale of ~a year.
* Reynolds Number: ratio of inertial force to viscous force in a fluid flow around an object (of dimension D). Higher the Reynolds number, the more small-scale eddies one will see; the largest-scale eddies are set by the dimension D. Reynolds number can be thought of the range of the scale of eddies--higher Reynolds number, less viscosity to damp eddy, and more small-scale eddies will form.
Bonvin, Caprini, Durrer
Same as above.
1112.3903
An estimate of the temporal fraction of cloud cover at San Pedro M'artier Observatory
Carasco, Carraminana, Sanchez, Avila, Cruz-Gonzalez
Find 82.4 % of the time the sky is clear of clouds at this site.
1112.3911
Galactic sources of high-energy neutrinos: Highlights
Vissani, Aharonian
Overview of high-energy neutrinos from galactic sources, transparent [?] to their gamma-ray emission [?]. Focus on young SNe remnants. Consider possibility of detecting neutrinos from other strong galactic gamma-ray sources, such as Vela Junior, Cygnus Region and Fermi Bubbles. Quantify the impact of large theta_13 on high-energy neutrino oscillations.
1112.3917
Detection of very high energy gamma-ray emission from NGC 1275 by the MAGIC telescopes
MAGIC collaboration, Lombardi, Colin, Hildebrand, Zandanel
VHE gamma-ray emission (E>100 GeV) from NGC 1275, the central radio galaxy of the Perseus cluster of galaxies. Fermi-LAT measured spectra above 100 MeV. Indicates a break or cut-off around ~10s GeV in the spectrum. E > 100 GeV does not show variability in the month timescale. Non-detection of radio galaxy IC 310. VHE has a variability timescale of ~a year.
* Reynolds Number: ratio of inertial force to viscous force in a fluid flow around an object (of dimension D). Higher the Reynolds number, the more small-scale eddies one will see; the largest-scale eddies are set by the dimension D. Reynolds number can be thought of the range of the scale of eddies--higher Reynolds number, less viscosity to damp eddy, and more small-scale eddies will form.
No comments:
Post a Comment