SN 2006gy: DISCOVERY OF THE MOST LUMINOUS
... However, there are reasons to suspect that the mass-loss properties of stars in the local universe may not be so different from these early stars. Namely, recent studies of line-driven winds from O-type stars and WR stars have shown that their winds are highly clumped, requiring that their mass-loss ...
... However, there are reasons to suspect that the mass-loss properties of stars in the local universe may not be so different from these early stars. Namely, recent studies of line-driven winds from O-type stars and WR stars have shown that their winds are highly clumped, requiring that their mass-loss ...
Post Common Envelope Binaries from SDSS. I: 101 white dwarf
... Real progress in our understanding of close binary evolution is most likely to arise from the analysis of post common envelope binaries (PCEBs) that are both numerous and well-understood in terms of their stellar components – such as PCEBs containing a white dwarf and a main sequence star1 . While d ...
... Real progress in our understanding of close binary evolution is most likely to arise from the analysis of post common envelope binaries (PCEBs) that are both numerous and well-understood in terms of their stellar components – such as PCEBs containing a white dwarf and a main sequence star1 . While d ...
FERMI GBM detections of four AXPs at soft gamma-rays
... (1998) measured the period and period derivative of SGR 1806-20. From these measurements, they found that the observed persistent X-ray flux of this SGR is two orders of magnitude higher than what can be explained from rotational energy loss, indicating that SGR 1806-20 is not rotation-powered. More ...
... (1998) measured the period and period derivative of SGR 1806-20. From these measurements, they found that the observed persistent X-ray flux of this SGR is two orders of magnitude higher than what can be explained from rotational energy loss, indicating that SGR 1806-20 is not rotation-powered. More ...
The Massive Star Population of Cygnus OB2
... stars have secondaries with known spectral types, although it is likely that there still remain a number of undiscovered binary companions in this sample. For objects with known companions it is possible to correct for the light of the secondary when using the observed photometry as long as the spec ...
... stars have secondaries with known spectral types, although it is likely that there still remain a number of undiscovered binary companions in this sample. For objects with known companions it is possible to correct for the light of the secondary when using the observed photometry as long as the spec ...
Lithium abundances in nearby FGK dwarf and subgiant stars
... aware of any prior analysis of differences in lithium abundances between the thin and thick disks, which can be investigated by studying stars that have experienced the least amount of lithium depletion. RAL’s data set includes also spectra of a number of old halo stars, which we can use to shed new ...
... aware of any prior analysis of differences in lithium abundances between the thin and thick disks, which can be investigated by studying stars that have experienced the least amount of lithium depletion. RAL’s data set includes also spectra of a number of old halo stars, which we can use to shed new ...
Microscopic vortex velocity in the inner crust and outer core of
... and dripped neutron superfluid interspersed with them is well established since the pioneering work of Negele & Vautherin (1973). The superfluid density inside a nucleus is found to be somewhat larger than the outside dripped superfluid, ρ in > ρ out , in most parts of the inner crust. This means th ...
... and dripped neutron superfluid interspersed with them is well established since the pioneering work of Negele & Vautherin (1973). The superfluid density inside a nucleus is found to be somewhat larger than the outside dripped superfluid, ρ in > ρ out , in most parts of the inner crust. This means th ...
Evidence of suppression of star formation by quasar
... identified. During the kinetic mode, also called radio jet or maintenance mode, the AGN luminosity is low and the feedback process is non-destructive. This mode keeps the balance between gas cooling and heating and is typically found in low redshift, massive galaxies. In the quasar mode (also called ...
... identified. During the kinetic mode, also called radio jet or maintenance mode, the AGN luminosity is low and the feedback process is non-destructive. This mode keeps the balance between gas cooling and heating and is typically found in low redshift, massive galaxies. In the quasar mode (also called ...
Polaris B, an optical companion of the Polaris (αUMi) system
... Since we can estimate a radius value for F3 V spectral-type main sequence near 1.38 R (Straižys 1982), therefore its luminosity is 3.868 L , and absolute magnitude MV = +3.30 mag. Using AV = 0.102 mag from Usenko et al. (2005a), we can obtain the distance D = 109.5 pc. This result has an ideal ag ...
... Since we can estimate a radius value for F3 V spectral-type main sequence near 1.38 R (Straižys 1982), therefore its luminosity is 3.868 L , and absolute magnitude MV = +3.30 mag. Using AV = 0.102 mag from Usenko et al. (2005a), we can obtain the distance D = 109.5 pc. This result has an ideal ag ...
The age of elliptical galaxies and bulges in a merger model The age
... The semi-analytic models we employ are described in detail in KWG and Kauffmann & White (1993). Application of the model to the evolution of the galaxy population in clusters at high redshift is discussed in Kauffmann (1995). Here we present a brief summary of that paper. An algorithm based on an ex ...
... The semi-analytic models we employ are described in detail in KWG and Kauffmann & White (1993). Application of the model to the evolution of the galaxy population in clusters at high redshift is discussed in Kauffmann (1995). Here we present a brief summary of that paper. An algorithm based on an ex ...
The keV–TeV connection in gamma-ray binaries
... The gamma-ray emission from astrophysical sources is arguably different from the emission in the rest of the electromagnetic spectrum because it cannot be generated by hot matter. High energy gamma radiation is therefore an indication that non-thermal processes, which are able to concentrate a large ...
... The gamma-ray emission from astrophysical sources is arguably different from the emission in the rest of the electromagnetic spectrum because it cannot be generated by hot matter. High energy gamma radiation is therefore an indication that non-thermal processes, which are able to concentrate a large ...
thesis
... is exhausted, the accretion rate from the disk onto the star drops. While the star contracts, its temperature increases and the developing stellar winds clear away the remaining material from the cloud. In the disk, planetesimals and finally planets are thought to be able to form. The star, which th ...
... is exhausted, the accretion rate from the disk onto the star drops. While the star contracts, its temperature increases and the developing stellar winds clear away the remaining material from the cloud. In the disk, planetesimals and finally planets are thought to be able to form. The star, which th ...
THE GREAT AGN DEBATE `AGN VS STARBURST
... 12. SMBH have a mass of between 105 and 1.8x 1010 solar masses. Most, if not all galaxies, including the Milky Way, are thought to host supermassive black holes at their centers. It’s generally considered that they are responsible for powering AGN. The Rev John Michell is credited with being the fir ...
... 12. SMBH have a mass of between 105 and 1.8x 1010 solar masses. Most, if not all galaxies, including the Milky Way, are thought to host supermassive black holes at their centers. It’s generally considered that they are responsible for powering AGN. The Rev John Michell is credited with being the fir ...
paper - Harvard-Smithsonian Center for Astrophysics
... that of the 235151.7 MHz transition for the outflow sources A, B, and C. Due to the lack of emission from the 235151.7 MHz line in the vicinity of source D, the 236216.7 MHz line was used instead to calculate line ratios. Fits to our data are presented as the χ 2 statistic p-value for each assumed v ...
... that of the 235151.7 MHz transition for the outflow sources A, B, and C. Due to the lack of emission from the 235151.7 MHz line in the vicinity of source D, the 236216.7 MHz line was used instead to calculate line ratios. Fits to our data are presented as the χ 2 statistic p-value for each assumed v ...
Physical Processes in the Interstellar Medium
... density and also freezes out on dust grains at very high densities, other tracers such as HCN or N2 H+ need to be used to study conditions within high density regions such as prestellar cores. We discuss the microphysics of the interaction between radiation and matter and the various heating and coo ...
... density and also freezes out on dust grains at very high densities, other tracers such as HCN or N2 H+ need to be used to study conditions within high density regions such as prestellar cores. We discuss the microphysics of the interaction between radiation and matter and the various heating and coo ...
CENTRAL STARS OF PLANETARY NEBULAE IN THE LARGE
... to model the background measured off target and subtracts it from the target spectrum. We found that, for our fainter objects, the background appeared to be overestimated with this method, particularly at shorter wavelengths (i.e., <1000 8). We therefore tried two other reductions. In the first, sub ...
... to model the background measured off target and subtracts it from the target spectrum. We found that, for our fainter objects, the background appeared to be overestimated with this method, particularly at shorter wavelengths (i.e., <1000 8). We therefore tried two other reductions. In the first, sub ...
