Pulsations in White Dwarfs
... of post-AGB objects; He-C-O in roughly comparable proportions) Low-degree (1,2), low- to mid-order g-mode pulsators Opacity-driven (classical kappa-mechanism) due to opaque high ions of C and O in the envelope ...
... of post-AGB objects; He-C-O in roughly comparable proportions) Low-degree (1,2), low- to mid-order g-mode pulsators Opacity-driven (classical kappa-mechanism) due to opaque high ions of C and O in the envelope ...
Star Formation in the Rosette Complex
... The pioneering observations by Gosachinskii & Khersonskii (1982) of the HI emission at 21 cm made with the RATAN-600 telescope revealed that the Rosette Complex and the Monoceros Loop were enclosed in a thin HI envelope 130 pc in diameter, possibly expanding at 20 km·s−1 , suggesting that the supern ...
... The pioneering observations by Gosachinskii & Khersonskii (1982) of the HI emission at 21 cm made with the RATAN-600 telescope revealed that the Rosette Complex and the Monoceros Loop were enclosed in a thin HI envelope 130 pc in diameter, possibly expanding at 20 km·s−1 , suggesting that the supern ...
THE SOFT STATE OF CYGNUS X-1 OBSERVED WITH
... Our choice of models is largely driven by pragmatic considerations. For the reflected emission, we use the XILLVER reflection model because it incorporates the effects of viewing angle (i.e., the disk inclination, i) on the observed reflection spectrum. We use the combination of XILLVER and RELCONV to ...
... Our choice of models is largely driven by pragmatic considerations. For the reflected emission, we use the XILLVER reflection model because it incorporates the effects of viewing angle (i.e., the disk inclination, i) on the observed reflection spectrum. We use the combination of XILLVER and RELCONV to ...
Systematic variation in the apparent burning area of thermonuclear
... of Astronomy and Maryland Astronomy Center for Theory and Computation, University of Maryland, College Park, MD 20742-2421, USA 3 Center for Stellar and Planetary Astrophysics, Monash University, Victoria 3800, Australia 2 Department ...
... of Astronomy and Maryland Astronomy Center for Theory and Computation, University of Maryland, College Park, MD 20742-2421, USA 3 Center for Stellar and Planetary Astrophysics, Monash University, Victoria 3800, Australia 2 Department ...
UNIT 4 - Galaxies XIV. The Milky Way A. Structure
... recent observations suggest that most, if not all, Quasars reside in a host galaxy ...
... recent observations suggest that most, if not all, Quasars reside in a host galaxy ...
3. Solar System Formation and Early Evolution
... observations of our galaxy (the Milky Way) and other galaxies tell us. The birthplace of stars are the so-called ‘‘molecular clouds’’, i.e., vast, cold volumes of gas (mostly molecular hydrogen and helium, and also complex organic molecules, with so far up to 11 C atoms: see Ehrenfreund and Charnley ...
... observations of our galaxy (the Milky Way) and other galaxies tell us. The birthplace of stars are the so-called ‘‘molecular clouds’’, i.e., vast, cold volumes of gas (mostly molecular hydrogen and helium, and also complex organic molecules, with so far up to 11 C atoms: see Ehrenfreund and Charnley ...
Massive quiescent galaxies at cosmic noon Robert Feldmann UC Berkeley
... stars atnoise rates ~1000 times possibility that some subtle systematic effe objects are as extreme asour Galaxy, that of very dusty the analysis, given the low signal-to-noise ed to have much• higher extremely luminous in sub-mm laxies of the same mass. We observed the galaxy, dubbed 1255–0, • few ...
... stars atnoise rates ~1000 times possibility that some subtle systematic effe objects are as extreme asour Galaxy, that of very dusty the analysis, given the low signal-to-noise ed to have much• higher extremely luminous in sub-mm laxies of the same mass. We observed the galaxy, dubbed 1255–0, • few ...
150 Million ly - Northern Michigan University
... • Dark Matter appears to be within and in the immediate space surrounding galaxies • The visible components appear to trace the locations of Dark Matter ...
... • Dark Matter appears to be within and in the immediate space surrounding galaxies • The visible components appear to trace the locations of Dark Matter ...
Evolution of the Highest Redshift Quasars
... – How closely tied are the earliest SBHs and galaxies? Or are we just picking up early starters in term of BH accretion in the most luminous quasars? ...
... – How closely tied are the earliest SBHs and galaxies? Or are we just picking up early starters in term of BH accretion in the most luminous quasars? ...
Star Formation in Disks: Spiral Arms, Turbulence, and Triggering
... triggering. Energy types include thermal, magnetic, turbulent, cosmic ray, and rotational. The first four are all comparable and equal to several tenths of an eV cm−3 . Rotational energy is much denser, several hundred eV cm−3 . Of the first four, only supersonic turbulence has been associated with st ...
... triggering. Energy types include thermal, magnetic, turbulent, cosmic ray, and rotational. The first four are all comparable and equal to several tenths of an eV cm−3 . Rotational energy is much denser, several hundred eV cm−3 . Of the first four, only supersonic turbulence has been associated with st ...
Propagation of Supernova Blast Waves through the ISM
... Multi-D is necessary to account for effects such as instabilities in the shock waves (Raleigh-Tayor, Richtmyer-Meshkov), consequences of asymmetries in the CSM or interactions with cloudlets present in the ambient medium. Ejecta clumps can be transported outward of the front shock by turbulence. 3D ...
... Multi-D is necessary to account for effects such as instabilities in the shock waves (Raleigh-Tayor, Richtmyer-Meshkov), consequences of asymmetries in the CSM or interactions with cloudlets present in the ambient medium. Ejecta clumps can be transported outward of the front shock by turbulence. 3D ...
ppt
... depending on the precise cosmological models as the expansion of the universe slows due to gravitational attraction of the matter within it • The current value of the Hubble constant is hotly debated, with two opposing camps generally getting values near the high and low ends of 50-100 km s-1/Mpc • ...
... depending on the precise cosmological models as the expansion of the universe slows due to gravitational attraction of the matter within it • The current value of the Hubble constant is hotly debated, with two opposing camps generally getting values near the high and low ends of 50-100 km s-1/Mpc • ...
L103 A NEW MILKY WAY DWARF SATELLITE IN CANES
... same area. Upper right: Binned spatial density of all stellar objects. The inner dotted circle marks a radius of 0⬚. 25, the middle circle a radius of 0⬚. 5, and the outermost circle a radius of 0⬚. 56. Bins are 0⬚. 05 # 0⬚. 05, smoothed with a Gaussian with an FWHM of 0⬚. 1. Lower left: CMD of all ...
... same area. Upper right: Binned spatial density of all stellar objects. The inner dotted circle marks a radius of 0⬚. 25, the middle circle a radius of 0⬚. 5, and the outermost circle a radius of 0⬚. 56. Bins are 0⬚. 05 # 0⬚. 05, smoothed with a Gaussian with an FWHM of 0⬚. 1. Lower left: CMD of all ...
M77 (NGC 1068)
... Galaxies who’s nuclei alone produce more radiation then the rest of the galaxy. The widely accepted model of an AGN galaxy is that it has a central super massive black hole as it’s engine. ...
... Galaxies who’s nuclei alone produce more radiation then the rest of the galaxy. The widely accepted model of an AGN galaxy is that it has a central super massive black hole as it’s engine. ...
Astronomy Astrophysics
... is small in area and has a very low field strength any alignment offset plays a proportionately higher role and as such the confidence in the value falls, leading to a ratio which is artificially high. The added benefit with this ratio method is that any underestimation of field has less of an effec ...
... is small in area and has a very low field strength any alignment offset plays a proportionately higher role and as such the confidence in the value falls, leading to a ratio which is artificially high. The added benefit with this ratio method is that any underestimation of field has less of an effec ...
doctoral thesis (Dissertation)
... and UV spectroscopy and through detailed physical simulations. Spectroscopic X-ray data is reduced and presented for two targets: The CTTS V4046 Sgr was observed with Chandra for 100 ks, using a high-resolution grating spectrometer. The lightcurve contains one flare and the He-like triplets of Si xi ...
... and UV spectroscopy and through detailed physical simulations. Spectroscopic X-ray data is reduced and presented for two targets: The CTTS V4046 Sgr was observed with Chandra for 100 ks, using a high-resolution grating spectrometer. The lightcurve contains one flare and the He-like triplets of Si xi ...
WFIRSTSurveyScience
... our knowledge of the initial mass function in young regions -- where the low mass objects are brighter by many orders of magnitude than they are on the main sequence -- down to and below the opacity limit for fragmentation within the molecular cloud. We see deeper into the mass function in these reg ...
... our knowledge of the initial mass function in young regions -- where the low mass objects are brighter by many orders of magnitude than they are on the main sequence -- down to and below the opacity limit for fragmentation within the molecular cloud. We see deeper into the mass function in these reg ...
Chemical Signatures in Dwarf Galaxies
... How these different types of galaxies are related to one another raises an interesting series of questions. Are dwarf gal axies related to protogalactic fragments, the low mass systems that formed in a L Cold Dark Matter (LCDM) Universe that later merged to build up the large spirals that we see to ...
... How these different types of galaxies are related to one another raises an interesting series of questions. Are dwarf gal axies related to protogalactic fragments, the low mass systems that formed in a L Cold Dark Matter (LCDM) Universe that later merged to build up the large spirals that we see to ...
SKA and VLBI synergies
... that the scientific targets will be imaged both in total intensity and polarisation with better detail than is possible today. Additionally, the accuracy of the source sizes obtained via model fitting will also benefit from the increased sensitivity [27]. Assuming observations at 5 GHz and observati ...
... that the scientific targets will be imaged both in total intensity and polarisation with better detail than is possible today. Additionally, the accuracy of the source sizes obtained via model fitting will also benefit from the increased sensitivity [27]. Assuming observations at 5 GHz and observati ...
From ATLASGAL to SEDIGISM: Towards a Complete 3D View of the
... 20 % of these filaments, preferentially within the ones with the largest mass-tolength ratios. Moreover, these filaments are predominantly aligned with the Galactic Plane, and associated with the spiral arms. This seems to indicate a direct link between star formation activity and large scale Galact ...
... 20 % of these filaments, preferentially within the ones with the largest mass-tolength ratios. Moreover, these filaments are predominantly aligned with the Galactic Plane, and associated with the spiral arms. This seems to indicate a direct link between star formation activity and large scale Galact ...
X-ray emission from supernova shock waves Tanja Kramer Nymark Department of Astronomy
... interaction with a circumstellar medium. In particular the reverse shock created by the interaction is investigated. In most Type IIL and Type IIn supernovae this shock is radiative, and due to the high temperature most of the radiation comes out as X-rays. A numerical model is presented which calcu ...
... interaction with a circumstellar medium. In particular the reverse shock created by the interaction is investigated. In most Type IIL and Type IIn supernovae this shock is radiative, and due to the high temperature most of the radiation comes out as X-rays. A numerical model is presented which calcu ...
"The Pulsar Menagerie" (pdf file)
... might be able to tell how many rocks splashed in—and how big they were. In space, the “rocks” are binary pairs of giant black holes at the cores of galaxies, and the “ripples” are gravitational waves. Long before they crash, the spiraling black holes churn the waters of spacetime. The waves, spannin ...
... might be able to tell how many rocks splashed in—and how big they were. In space, the “rocks” are binary pairs of giant black holes at the cores of galaxies, and the “ripples” are gravitational waves. Long before they crash, the spiraling black holes churn the waters of spacetime. The waves, spannin ...
THE YELLOW SUPERGIANT PROGENITOR OF THE TYPE II
... panel: the spectroscopic evolution of SN 2011dh. Blue (dashed) lines mark the He i λλ6678, 7065, 7281 lines. Red (dotted) lines mark Hα at the rest wavelength and at −12, 500 km s−1 . All spectra and photometry have been corrected for reddening using the extinction law of Cardelli et al. (1989) and ...
... panel: the spectroscopic evolution of SN 2011dh. Blue (dashed) lines mark the He i λλ6678, 7065, 7281 lines. Red (dotted) lines mark Hα at the rest wavelength and at −12, 500 km s−1 . All spectra and photometry have been corrected for reddening using the extinction law of Cardelli et al. (1989) and ...
PDF only
... Figure 2 – (a) Measured masses of neutron stars in binary systems; the data are divided according to the nature of the companion star in the system (from Ref. [3-b]). (b) Measured surface temperatures of isolated neutron stars; the ages reported in abscissa are obtained from the rotating dipole mode ...
... Figure 2 – (a) Measured masses of neutron stars in binary systems; the data are divided according to the nature of the companion star in the system (from Ref. [3-b]). (b) Measured surface temperatures of isolated neutron stars; the ages reported in abscissa are obtained from the rotating dipole mode ...
Active Galactic Nuclei at kiloparsec scales and their cosmological
... found that the incidence of disturbed morphologies is not significantly enhanced over the general population of galaxies (e.g., [12]), leaving secular processes as the most likely triggering mechanism at such luminosities [48]. Thus, it seems that AGN of different luminosities are triggered in diffe ...
... found that the incidence of disturbed morphologies is not significantly enhanced over the general population of galaxies (e.g., [12]), leaving secular processes as the most likely triggering mechanism at such luminosities [48]. Thus, it seems that AGN of different luminosities are triggered in diffe ...
Astrophysical X-ray source
Astrophysical X-ray sources are astronomical objects with physical properties which result in the emission of X-rays.There are a number of types of astrophysical objects which emit X-rays, from galaxy clusters, through black holes in active galactic nuclei (AGN) to galactic objects such as supernova remnants, stars, and binary stars containing a white dwarf (cataclysmic variable stars and super soft X-ray sources), neutron star or black hole (X-ray binaries). Some solar system bodies emit X-rays, the most notable being the Moon, although most of the X-ray brightness of the Moon arises from reflected solar X-rays. A combination of many unresolved X-ray sources is thought to produce the observed X-ray background. The X-ray continuum can arise from bremsstrahlung, either magnetic or ordinary Coulomb, black-body radiation, synchrotron radiation, inverse Compton scattering of lower-energy photons be relativistic electrons, knock-on collisions of fast protons with atomic electrons, and atomic recombination, with or without additional electron transitions.Furthermore, celestial entities in space are discussed as celestial X-ray sources. The origin of all observed astronomical X-ray sources is in, near to, or associated with a coronal cloud or gas at coronal cloud temperatures for however long or brief a period.