Wind Opacity Issues
... OFH2006 shows this plot of wind opacity for four stars (below), from “detailed” wind modeling using PoWR. It appears that the only K-shell edge is that of (a single ion state of) nitrogen. This seems pretty crude. And it makes me wonder what elements are included in the calculation of the overall op ...
... OFH2006 shows this plot of wind opacity for four stars (below), from “detailed” wind modeling using PoWR. It appears that the only K-shell edge is that of (a single ion state of) nitrogen. This seems pretty crude. And it makes me wonder what elements are included in the calculation of the overall op ...
A Massive Galaxy in its Core Formation Phase Three Billion Years
... Most massive galaxies are thought to have formed their dense stellar cores at early cosmic epochs.1–3 However, cores in their formation phase have not yet been observed. Previous studies have found galaxies with high gas velocity dispersions4 or small apparent sizes5–7 but so far no objects have bee ...
... Most massive galaxies are thought to have formed their dense stellar cores at early cosmic epochs.1–3 However, cores in their formation phase have not yet been observed. Previous studies have found galaxies with high gas velocity dispersions4 or small apparent sizes5–7 but so far no objects have bee ...
Clumpy wind accretion in supergiant neutron star high mass X
... density and velocity structures in the wind, where dense shells are formed relatively close to the star during a first stage of unstable growth of the LDI. The dense shells have rather small radial extent, low electron temperatures (T e ∼10 kK) and contain the bulk of the wind mass. The colloquial t ...
... density and velocity structures in the wind, where dense shells are formed relatively close to the star during a first stage of unstable growth of the LDI. The dense shells have rather small radial extent, low electron temperatures (T e ∼10 kK) and contain the bulk of the wind mass. The colloquial t ...
Red Supergiants as Cosmic Abundance Probes
... It is well known that massive star clusters with ages between 7–50 Myr may contain dozens of RSGs. If such a cluster was at a distance so great that it was totally unresolved and appeared as a point source, and we mistook it for a single abnormally bright RSG, what would we see? ...
... It is well known that massive star clusters with ages between 7–50 Myr may contain dozens of RSGs. If such a cluster was at a distance so great that it was totally unresolved and appeared as a point source, and we mistook it for a single abnormally bright RSG, what would we see? ...
Star Wreck
... SECS type, their effect is negligible. If, however, they are SENS, they consume the white dwarf from the inside, just like in the case of a neutron star. The white dwarfs also become unstable when their masses become less than 2.2 × 10−3 M⊙ , at which ...
... SECS type, their effect is negligible. If, however, they are SENS, they consume the white dwarf from the inside, just like in the case of a neutron star. The white dwarfs also become unstable when their masses become less than 2.2 × 10−3 M⊙ , at which ...
Galaxies over the Latter Half of Cosmic Time
... eventually spawned the first generation of stars. Over billions of years, supernova explosions enriched the mix with oxygen, carbon, iron, and other elements that form only inside stars. These heavy elements are necessary to make planets such as Earth. The local gas consumed by star formation was re ...
... eventually spawned the first generation of stars. Over billions of years, supernova explosions enriched the mix with oxygen, carbon, iron, and other elements that form only inside stars. These heavy elements are necessary to make planets such as Earth. The local gas consumed by star formation was re ...
High energy processes in young stellar objects and high-mass X
... 4.2 Fermi observational data . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4.3 Fermi /LAT data analysis . . . . . . . . . . . . . . . . . . . . . . . . . . . 4.4 Results . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4.5 Discussion . . . . . . . . . . . . . . . ...
... 4.2 Fermi observational data . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4.3 Fermi /LAT data analysis . . . . . . . . . . . . . . . . . . . . . . . . . . . 4.4 Results . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4.5 Discussion . . . . . . . . . . . . . . . ...
radiation and matter interaction in strong magnetic field of accreting
... This thesis focuses on the theoretical study of radiation and matter interaction in the vicinity of strongly magnetized neutron stars (NSs). NSs give us a unique possibility to study physical processes in such extreme conditions (huge temperatures, densities and magnetic fields) which by no means ca ...
... This thesis focuses on the theoretical study of radiation and matter interaction in the vicinity of strongly magnetized neutron stars (NSs). NSs give us a unique possibility to study physical processes in such extreme conditions (huge temperatures, densities and magnetic fields) which by no means ca ...
driving galaxy evolution since z=1
... • Groups accelerate the termination of star formation at z<1 For reasons that are still not understood. ...
... • Groups accelerate the termination of star formation at z<1 For reasons that are still not understood. ...
Dark Matter Spiral Structure Basic Galaxy Morphology Disk Galaxy Rotation Curves:
... - non-baryonic dark matter currently unknown The Milky Way halo probably contains some baryonic dark matter - brown dwarfs + stellar remnants accompanying the known population of low mass stars. This uncontroversial component of dark matter is not enough is the remainder baryonic or non-baryonic? ...
... - non-baryonic dark matter currently unknown The Milky Way halo probably contains some baryonic dark matter - brown dwarfs + stellar remnants accompanying the known population of low mass stars. This uncontroversial component of dark matter is not enough is the remainder baryonic or non-baryonic? ...
models for low-mass x-ray binaries in the elliptical
... it can be used as a probe of the galaxy’s merger history. In addition, the presence of faint primordial X-ray binaries in an old galactic component is addressed, predicting for the first time that this population of X-ray binaries should be observable in old galaxies such as the two ellipticals NGC ...
... it can be used as a probe of the galaxy’s merger history. In addition, the presence of faint primordial X-ray binaries in an old galactic component is addressed, predicting for the first time that this population of X-ray binaries should be observable in old galaxies such as the two ellipticals NGC ...
A galaxy rapidly forming stars 700 million years after the Big Bang at
... that a typical galaxy at z < 7 has SFR 5 10 M[ yr21; the measured SFR of z8_GND_5296 is a factor of more than 30 times greater. If this SFR function is accurate, the expected space density per co-moving Mpc3 for this galaxy would be =1025. The implied rarity of this galaxy could indicate that it is ...
... that a typical galaxy at z < 7 has SFR 5 10 M[ yr21; the measured SFR of z8_GND_5296 is a factor of more than 30 times greater. If this SFR function is accurate, the expected space density per co-moving Mpc3 for this galaxy would be =1025. The implied rarity of this galaxy could indicate that it is ...
Modeling non-thermal emission from stellar bow shocks
... detected in the IR (Comerón & Pasquali 2007) and in radio (Benaglia et al. 2010). Both observations are coincident and extensive. Assuming the velocity of this star is 67 km s−1 (Kobulnicky et al. 2010), the mass-loss rate 10−5 M⊙ yr−1 (Markova et al. 2004; Repolust et al. 2004), the stellar wind v ...
... detected in the IR (Comerón & Pasquali 2007) and in radio (Benaglia et al. 2010). Both observations are coincident and extensive. Assuming the velocity of this star is 67 km s−1 (Kobulnicky et al. 2010), the mass-loss rate 10−5 M⊙ yr−1 (Markova et al. 2004; Repolust et al. 2004), the stellar wind v ...
discovery of Quasars
... Mostly Normal Galaxies (e.g. Thermal emission of spiral galaxies like the MW) “Stars” with strange broad emission lines! ...
... Mostly Normal Galaxies (e.g. Thermal emission of spiral galaxies like the MW) “Stars” with strange broad emission lines! ...
Targets for Small Telescopes
... primary being slightly larger and brighter than the secondary. Different observers see the secondary as different colours. The colours I have mentioned previously, Yellow and Pale Yellow/White are consistent with the spectral types, sometimes I see the secondary as having a pale green or emerald ton ...
... primary being slightly larger and brighter than the secondary. Different observers see the secondary as different colours. The colours I have mentioned previously, Yellow and Pale Yellow/White are consistent with the spectral types, sometimes I see the secondary as having a pale green or emerald ton ...
Vicky Kaspi Chandra Anomalous X-ray Pulsars Fotis Gavriil
... • Lx powered by internal heating due to B field • Thermal X-rays scattered by currents in twisted magnetosphere (Thompson, Lyutikov & Kulkarni 2002) ...
... • Lx powered by internal heating due to B field • Thermal X-rays scattered by currents in twisted magnetosphere (Thompson, Lyutikov & Kulkarni 2002) ...
History of IGM (C. Carilli)
... First tests (4 prototypes): Q1, Q2 2005 First experiments (100-200 hr): D array, Q4 2005 Large proposal (500 hr): D array, Q1 2007 ...
... First tests (4 prototypes): Q1, Q2 2005 First experiments (100-200 hr): D array, Q4 2005 Large proposal (500 hr): D array, Q1 2007 ...
Lecture 2. Thermal evolution and surface emission of
... to a crystalline/gapless color-superconducting state ...
... to a crystalline/gapless color-superconducting state ...
"Galaxies and the Universe" Lesson Outline answers
... c. Scientists can measure the speed at which galaxies move away from Earth by observing wavelengths of light. ...
... c. Scientists can measure the speed at which galaxies move away from Earth by observing wavelengths of light. ...
Chapter 16 Galaxies and Dark Matter
... large compared to the size of the galaxies themselves, and galactic collisions are frequent. The “cartwheel” galaxy on the left appears to be the result of a head-on collision with another galaxy, perhaps one of those on the right. ...
... large compared to the size of the galaxies themselves, and galactic collisions are frequent. The “cartwheel” galaxy on the left appears to be the result of a head-on collision with another galaxy, perhaps one of those on the right. ...
BREATHING IN LOW MASS GALAXIES: A STUDY - N
... Given their susceptibility to galactic “weather”, the cool baryonic content of dwarf galaxies should fluctuate, not just from galaxy to galaxy, but within an individual galaxy as a function of time. The expected temporal variations in the amount of cool gas should be accompanied by variations in the ...
... Given their susceptibility to galactic “weather”, the cool baryonic content of dwarf galaxies should fluctuate, not just from galaxy to galaxy, but within an individual galaxy as a function of time. The expected temporal variations in the amount of cool gas should be accompanied by variations in the ...
Absorption of high-energy gamma rays in Cygnus X-3
... Conclusions. The lack of an absorption feature in the GeV emission indicates that high-energy gamma rays should be located at a minimum distance ∼108 −1010 cm from the compact object. The gamma-ray emission is unlikely to have a coronal origin. Key words. radiation mechanisms: non-thermal – stars: i ...
... Conclusions. The lack of an absorption feature in the GeV emission indicates that high-energy gamma rays should be located at a minimum distance ∼108 −1010 cm from the compact object. The gamma-ray emission is unlikely to have a coronal origin. Key words. radiation mechanisms: non-thermal – stars: i ...
Resources: - Real Science
... describe it in multiple reports in the Astrophysical Journal and Monthly Notices of the Royal Astronomical Society. The magnetar is in a star cluster about 15 000 light-years away, in the Ara constellation. This is in the southern hemisphere. The magnetar goes by the official name of CXOU J164710.2- ...
... describe it in multiple reports in the Astrophysical Journal and Monthly Notices of the Royal Astronomical Society. The magnetar is in a star cluster about 15 000 light-years away, in the Ara constellation. This is in the southern hemisphere. The magnetar goes by the official name of CXOU J164710.2- ...
The title of my PDF
... of activity that will emit synchrotron radiation if subject to an external magnetic field. This naturally gives us an exponential fall-off time once neutron captures stop, which as discussed above, can be much later in the expansion than traditionally expected in the r-process due to the high densit ...
... of activity that will emit synchrotron radiation if subject to an external magnetic field. This naturally gives us an exponential fall-off time once neutron captures stop, which as discussed above, can be much later in the expansion than traditionally expected in the r-process due to the high densit ...
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.