ROSAT Observations of the Pleiades. I. X-Ray Characteristics of a Coeval Stellar Population

1996 ◽  
Vol 102 ◽  
pp. 75 ◽  
Author(s):  
G. Micela ◽  
S. Sciortino ◽  
V. Kashyap ◽  
F. R., Jr. Harnden ◽  
R. Rosner
Keyword(s):  
Stellar Population ◽  
X Ray

scholarly journals Stellar population properties for a sample of hard X-ray AGNs

2013 ◽  
Vol 556 ◽  
pp. A135 ◽  
Author(s):  
L. Morelli ◽  
V. Calvi ◽  
N. Masetti ◽  
P. Parisi ◽  
R. Landi ◽  
...  
Keyword(s):  
Stellar Population ◽  
X Ray

scholarly journals Galactic Centers – Ours and Other Galaxies'

1989 ◽  
Vol 136 ◽  
pp. 21-35
Author(s):  
G. H. Rieke
Keyword(s):  
Stellar Population ◽  
Local Group ◽  
Galactic Center ◽  
Galactic Nuclei ◽  
X Ray ◽  
Galactic Centers ◽  
Modest Level

Viewed from outside the Local Group, the Galactic Center would be a paragon of ordinariness, both with regard to its stellar population and its nonstellar emission in the radio, infrared, and X-ray.Nonetheless, at a very modest level it shows evidence for many of the processes that we believe dominate the properties of exotic galactic nuclei.

scholarly journals Thermonuclear Processes on Accreting Neutron Stars

1981 ◽  
Vol 93 ◽  
pp. 207-227
Author(s):  
Paul C. Joss
Keyword(s):  
Spatial Distribution ◽  
Neutron Stars ◽  
Time Scales ◽  
Decay Time ◽  
Stellar Population ◽  
Effective Radius ◽  
X Ray ◽  
Burst Maximum ◽  
Many Sources ◽  
S Peak

The observed properties of X-ray burst sources have recently been reviewed by Lewin and Clark (1980) and Lewin and Joss (1980). About thirty-five such sources are presently known, and they have a spatial distribution reminiscent of stellar Population II (see Figure 1). The salient features of these sources include burst rise times of ≲ls, decay time scales of ~3–100 s, peak luminosities of ~1039 ergs per burst, spectra that can generally be well fitted by blackbody emission from a surface with a constant effective radius of ~10 km and a peak temperature of ~3 × 107 K, and “tails” of softer X-ray emission that may persist for several minutes after the burst maximum. Profiles of bursts from some typical burst sources are shown in Figure 2. The intervals between bursts from a given source may be regular or erratic and are typically in the range of ~104−105 s; many sources undergo burst-inactive phases that can last for weeks or months. Most burst sources are also sources of persistent X-ray emission, and the ratio of average persistent luminosity to time-averaged burst luminosity is typically ~102 during burst-active phases. (The properties of the “Rapid Burster,” MXB1730-335, are different from those of all other known burst sources and will be discussed separately in §VI below.) There are few correlations among the burst flux, burst intervals, and persistent X-ray flux from any given source, and the detailed burst shapes vary from one source to another and often vary with time in a given source.

scholarly journals The X-ray stellar population of the LMC

2008 ◽  
Vol 4 (S256) ◽  
pp. 20-29 ◽  
Author(s):  
Yaël Nazé
Keyword(s):  
Stellar Population ◽  
Main Sequence ◽  
Massive Stars ◽  
High Energy ◽  
Magellanic Clouds ◽  
X Rays ◽  
X Ray ◽  
Energy Domain ◽  
X Ray Binaries

AbstractIn the study of stars, the high energy domain occupies a place of choice, since it is the only one able to directly probe the most violent phenomena: indeed, young pre-main sequence objects, hot massive stars, or X-ray binaries are best revealed in X-rays. However, previously available X-ray observatories often provided only crude information on individual objects in the Magellanic Clouds. The advent of the highly efficient X-ray facilities XMM-Newton and Chandra has now dramatically increased the sensitivity and the spatial resolution available to X-ray astronomers, thus enabling a fairly easy determination of the properties of individual sources in the LMC.

A study of the stellar population in the LYNDS 1641 dark cloud. IV - The Einstein X-ray sources

1990 ◽  
Vol 362 ◽  
pp. 168 ◽  
Author(s):  
Karen M. Strom ◽  
Stephen E. Strom ◽  
Francis P. Wilkin ◽  
Luis Carrasco ◽  
Irene Cruz-Gonzalez ◽  
...  
Keyword(s):  
Stellar Population ◽  
Dark Cloud ◽  
X Ray

scholarly journals A Survey of X-ray Point Sources in the Magellanic Clouds

1999 ◽  
Vol 192 ◽  
pp. 100-103
Author(s):  
A. P. Cowley ◽  
P. C. Schmidtke ◽  
V. A. Taylor ◽  
T.K. McGrath ◽  
J. B. Hutchings ◽  
...  
Keyword(s):  
Stellar Population ◽  
Population Based ◽  
Magellanic Clouds ◽  
Point Sources ◽  
High Mass ◽  
Be Stars ◽  
X Ray ◽  
The Galaxy ◽  
Low Mass ◽  
X Ray Binaries

In this study we compare the global populations of stellar X-ray sources in the LMC, SMC, and the Galaxy. After removing foreground stars and background AGN from the samples, the relative numbers of the various types of X-ray point sources within the LMC and SMC are similar, but differ markedly from those in the Galaxy. The Magellanic Clouds are rich in high-mass X-ray binaries (HMXB), especially those containing rapidly rotating Be stars. However, the LMC and SMC both lack the large number of low-mass X-ray binaries (LMXB) found in the Milky Way, which are known to represent a very old stellar population based on their kinematics, chemical composition, and spatial distribution.

scholarly journals Models for the Evolution of X-Ray Binaries in a Young Stellar Population

2005 ◽  
Vol 1 (S230) ◽  
pp. 417-422 ◽  
Author(s):  
M. Eracleous ◽  
M. S. Sipior ◽  
S. Sigurdsson
Keyword(s):  
Stellar Population ◽  
X Ray ◽  
X Ray Binaries

scholarly journals X-ray emission from the stellar population in M 32

2007 ◽  
Vol 473 (3) ◽  
pp. 783-789 ◽  
Author(s):  
M. Revnivtsev ◽  
E. Churazov ◽  
S. Sazonov ◽  
W. Forman ◽  
C. Jones
Keyword(s):  
Stellar Population ◽  
X Ray

scholarly journals AGN feedback and the origin and fate of the hot gas in early-type galaxies

2018 ◽  
Vol 14 (S342) ◽  
pp. 97-100
Author(s):  
Silvia Pellegrini ◽  
Luca Ciotti ◽  
Andrea Negri ◽  
Jeremiah P. Ostriker
Keyword(s):  
Stellar Population ◽  
Gas Content ◽  
Large Set ◽  
Early Type ◽  
X Ray ◽  
Hot Gas ◽  
Hydrodynamical Simulations ◽  
Consistent Treatment ◽  
The Impact ◽  
Recycled Material

AbstractWe present the results of two-dimensional, grid-type hydrodynamical simulations, with parsec-scale central resolution, for the evolution of the hot gas in isolated early-type galaxies (ETGs). The simulations include a physically self-consistent treatment of the mechanical (from winds) and radiative AGN feedback, and were run for a large set of realistic galaxy models. AGN feedback proves to be very important to maintain massive ETGs in a time-averaged quasi-steady state, keeping the star formation at a low level, and the central black hole mass on observed scaling relations. A comparison with recent determinations of the X-ray properties of ETGs in the local universe shows that, at later epochs, AGN feedback does not dramatically alter the gas content originating in stellar recycled material. Thus, the present-day X-ray luminosity is not a robust diagnostic of the impact of AGN activity, within a scenario where the hot gas mostly originates from the stellar population.

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