Not a white christmas but a windy one: Razoumov, Westmoquette et al, Rubin et al, Vanzella et al, Crenshaw et al, and Kobulnicky et al are all wind-related papers or preprints (and mainly on galactic winds). Another paper of particular note is Welsh et al's amazing 3-D mapping of the local neutral ISM (within 300 pc) using NaI and CaII absorption line spectroscopy toward 1857 nearby early-type stars.
Galaxies and Starbursts
Damped Lyα Absorber Kinematics and Outflows from Starburst GalaxiesRazoumov, Alexei O., 2009, The Astrophysical Journal, Volume 707, Issue 1, pp. 738-749.
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HTMLVLT/FLAMES-ARGUS observations of stellar wind-ISM cloud interactions in NGC 6357Westmoquette, M. S.; Slavin, J. D.; Smith, L. J.; Gallagher, J. S., III, 2009, MNRAS, in press
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PAH processing in a hot gasE. R. Micelotta, A. P. Jones, A. G. G. M. Tielens,
arXiv:0912.1595 [ps, pdf, other]Comments: 16 pages, 11 figures, accepted for publication in Astronomy and Astrophysics
From their abstract: "The PAH lifetime in a tenuous hot gas (n_H ~ 0.01 cm^-3, T ~ 10^7 K), typical of the coronal gas in galactic outflows, is found to be about thousand years, orders of magnitude shorter than the typical lifetime of such objects. Conclusions: In a hot gas, PAHs are principally destroyed by electron collisions and not by the absorption of X-ray photons from the hot gas. The resulting erosion of PAHs occurs via C_2 loss from the periphery of the molecule, thus preserving the aromatic structure. The observation of PAH emission from a million degree, or more, gas is only possible if the emitting PAHs are ablated from dense, entrained clumps that have not yet been exposed to the full effect of the hot gas."The Persistence of Cool Galactic Winds in High Stellar Mass Galaxies Between z~1.4 and ~1Kate H. R. Rubin, Benjamin J. Weiner, David C. Koo, Crystal L. Martin, J. Xavier Prochaska, Alison L. Coil, Jeffrey A. Newman,
arXiv:0912.2343 [ps, pdf, other]Comments: Submitted to ApJ. 25 pages, 19 figures, Figure 2 reduced in resolution. Uses emulateapj format
From their abstract: "We present an analysis of the MgII 2796, 2803 and FeII 2586, 2600 absorption line profiles in coadded spectra of 468 galaxies at 0.7 < z < 1.5. ... The outflows
have hydrogen column densities N(H) > 10^19.3 cm^-2, and extend to velocities
of ~500 km/s. While galaxies with SFR > 10 Msun/yr host strong outflows in both
this and the W09 sample, we do not detect outflows in lower-SFR (i.e., log
M_*/Msun < 10.5) galaxies at lower redshifts. Using a simple galaxy evolution
model which assumes exponentially declining SFRs, we infer that strong outflows
persist in galaxies with log M_*/Msun > 10.5 as they age between z=1.4 and z~1,
presumably because of their high absolute SFRs. Finally, using high resolution
HST/ACS imaging in tandem with our spectral analysis, we find evidence for a
weak trend (at 1 sigma significance) of increasing outflow absorption strength
with increasing galaxy SFR surface density."The unusual NIV]-emitter galaxy GDS J033218.92-275302.7: star formation or AGN-driven winds from a massive galaxy at z=5.56E. Vanzella, A. Grazian, M. Hayes, L. Pentericci, D. Schaerer, M. Dickinson, S. Cristiani, M. Giavalisco, A. Verhamme, M. Nonino, P. Rosati,
arXiv:0912.3007 [ps, pdf, other]Comments: 13 pages, 9 figures. Accepted for publication in Astronomy and Astrophysics
The central energy source of 70micron-selected galaxies: Starburst or AGN?M. Symeonidis, D. Rosario, A. Georgakakis, J. Harker, E. S. Laird, M. J. Page
Comments: 20 pages, 14 figures, accepted for publication in MNRAS
It is starbursts.Model analysis of the very high energy detections of the starburst galaxies M82 and NGC 253
E. de Cea del Pozo, D. F. Torres, A. Y. Rodriguez, O. Reimer,
arXiv:0912.3497 [ps, pdf, other]Comments: 6 pages, 3 figures, 2 tables, 2009 Fermi Symposium, eConf Proceedings C091122
Black Holes and AGN
The Geometry of Mass Outflows and Fueling Flows in the Seyfert 2 Galaxy Mrk 3D.M. Crenshaw, S.B. Kraemer, H.R. Schmitt, Y.L. Jaffe, R.P. Deo, N.R. Collins, T.C. Fischer,
arXiv:0912.2420 [ps, pdf, other]Comments: 22 page, 7 figures, accepted for publication in the Astronomical Journal
Their abstract: We present a study of the resolved emission-line regions and an inner dust/gas disk in the Seyfert 2 galaxy Mrk 3, based on Hubble Space Telescope observations. We show that the extended narrow-line region (ENLR), spanning ~4 kpc, is defined by the intersection of the ionizing bicone of radiation from the AGN and the inner disk, which is not coplanar with the large-scale stellar disk. This intersection leads to different position and opening angles of the ENLR compared to the narrow-line region (NLR). A number of emission-line arcs in the ENLR appear to be continuations of dust lanes in the disk, supporting this geometry. The NLR, which consists of outflowing emission-line knots spanning the central ~650 pc, is in the shape of a backwards S. This shape may arise from rotation of the gas, or it may trace the original fueling flow close to the nucleus that was ionized after the AGN turned on."
Stars, Supernovae and Planets
OB Stars & Stellar Bowshocks in Cygnus-X: A Novel Laboratory Estimating Stellar Mass Loss RatesHenry A. Kobulnicky, Ian J. Gilbert, Daniel C. Kiminki,
arXiv:0912.1314 [ps, pdf, other]
Comments: 49 pages, 19 figures; Accepted for publication in ApJ; full-resolution color figure version available at
this http URL; comments invited
CoRoT-7 b: Super-Earth or Super-Io?Rory Barnes, Sean N. Raymond, Richard Greenberg, Brian Jackson, Nathan A. Kaib,
arXiv:0912.1337 [ps, pdf, other]Comments: 13 pages, 3 figures, accepted to ApJ Letters
The simultaneous formation of massive stars and stellar clustersRowan J. Smith, Steven Longmore and Ian Bonnell, 2009, MNRAS, 400, 1775
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Updated stellar yields from Asymptotic Giant Branch modelsAmanda I. Karakas,
arXiv:0912.2142 [ps, pdf, other]Comments: Accepted for publication in MNRAS; 15 pages
New 3-D gas density maps of NaI and CaII interstellar absorption within 300pcBarry Y. Welsh, Rosine Lallement, Jean-Luc Vergely, Severine Raimond,
arXiv:0912.3040 [ps, pdf, other]Comments: A&A accepted
The NaI and CaII distributions are quite different. A very impressive piece of work.
Numerical Methods and Theoretical Astrophysics
Astrophysical turbulenceAxel Brandenburg, Aake Nordlund,
arXiv:0912.1340 [ps, pdf, other]
Detailed Decomposition of Galaxy Images. II. Beyond Axisymmetric ModelsChien Y. Peng, Luis C. Ho, Chris D. Impey, Hans-Walter Rix,
arXiv:0912.0731 [ps, pdf, other]
Dynamical Models for the Formation of Elephant Trunks in H II RegionsJonathan Mackey, Andrew J. Lim,
arXiv:0912.1499 [ps, pdf, other]
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