The Current Status of Galaxy Formation
... dark matter is found to be excessive in barred galaxies and in dwarfs. The resolution to all of these difficulties must lie in feedback. There are various flavors of feedback that span the range of processes including reionization at very high redshift, supernova (SN) explosions, tidal stripping and ...
... dark matter is found to be excessive in barred galaxies and in dwarfs. The resolution to all of these difficulties must lie in feedback. There are various flavors of feedback that span the range of processes including reionization at very high redshift, supernova (SN) explosions, tidal stripping and ...
Star Captures by Quasar Accretion Disks: A Possible Explanation of
... are captured their orbits are immediately replenished by relaxation processes. The slope of this relation is in good agreement with the observations (see also Merritt & Poon 2003). However, in this model black holes do not grow by gas accretion, so the similarity of the black hole mass density and t ...
... are captured their orbits are immediately replenished by relaxation processes. The slope of this relation is in good agreement with the observations (see also Merritt & Poon 2003). However, in this model black holes do not grow by gas accretion, so the similarity of the black hole mass density and t ...
Lithium abundances for 185 main-sequence stars
... resolution spectra of 130 stars and a reanalysis of data for 55 stars from Lambert et al. (1991). The survey takes advantage of improved photometric and spectroscopic determinations of effective temperature and metallicity as well as mass and age derived from Hipparcos absolute magnitudes, offering ...
... resolution spectra of 130 stars and a reanalysis of data for 55 stars from Lambert et al. (1991). The survey takes advantage of improved photometric and spectroscopic determinations of effective temperature and metallicity as well as mass and age derived from Hipparcos absolute magnitudes, offering ...
Astronomy 305/Frontiers in Astronomy - Fermi Gamma
... Chandra observations show link to hypernova model when hot iron-filled gas is detected from GRB 991216 ...
... Chandra observations show link to hypernova model when hot iron-filled gas is detected from GRB 991216 ...
Extragalactic Astronomical Masers I
... for Light Amplification by Stimulated Emission of Radiation. Laser is an artificial light and it is very different from other lights in that a laser light is highly collimated and coherently emits in space. Similarly, maser emits very narrow and intense emission at microwave or radio wavelengths ove ...
... for Light Amplification by Stimulated Emission of Radiation. Laser is an artificial light and it is very different from other lights in that a laser light is highly collimated and coherently emits in space. Similarly, maser emits very narrow and intense emission at microwave or radio wavelengths ove ...
Time evolution and rotation of starspots on CoRoT
... provides unambiguous information on the longitude of the corresponding spot. When the spot latitude is fixed a priori, the radius and the intensity of the spot may show some degree of degeneracy, but in the case of a highly accurate light curve, such as for CoRoT-2, they are independently constraine ...
... provides unambiguous information on the longitude of the corresponding spot. When the spot latitude is fixed a priori, the radius and the intensity of the spot may show some degree of degeneracy, but in the case of a highly accurate light curve, such as for CoRoT-2, they are independently constraine ...
Advanced aspects of radiation protection in the use of particle
... distance of 100 cm. ............................................................................... 156 ...
... distance of 100 cm. ............................................................................... 156 ...
ABSTRACT Stellar feedback, star formation and
... Star formation can potentially occur anywhere in the disk between 2.5 < r < 8.5 pc (our main region for analysis), whenever a cell’s density exceeds nH > 100 cm−3 and its temperature T < 3000 K. Since nH > 100 cm−3 is the observed average density for a GMC, in reality star formation would occur at m ...
... Star formation can potentially occur anywhere in the disk between 2.5 < r < 8.5 pc (our main region for analysis), whenever a cell’s density exceeds nH > 100 cm−3 and its temperature T < 3000 K. Since nH > 100 cm−3 is the observed average density for a GMC, in reality star formation would occur at m ...
CHARACTERIZING THE COOL KOIs. III. KOI 961: A SMALL STAR
... less than 1% chance that any one of the transiting signals is due to a background or hierarchical eclipsing binary, validating the planetary nature of the transits. The best-fitting radii for all three planets are less than 1 R⊕ , with KOI 961.03 being Mars-sized (RP = 0.57 ± 0.18 R⊕ ), and they rep ...
... less than 1% chance that any one of the transiting signals is due to a background or hierarchical eclipsing binary, validating the planetary nature of the transits. The best-fitting radii for all three planets are less than 1 R⊕ , with KOI 961.03 being Mars-sized (RP = 0.57 ± 0.18 R⊕ ), and they rep ...
THE GREAT AGN DEBATE `AGN VS STARBURST
... versions of Seyfert Type 1 galaxy. They show strong optical continuum emission, Xray continuum emission, and broad and narrow optical emission lines. Some astronomers use the term QSO for this object reserving 'quasar' for radio-loud objects, while others use the terminology radio-quiet and radio-lo ...
... versions of Seyfert Type 1 galaxy. They show strong optical continuum emission, Xray continuum emission, and broad and narrow optical emission lines. Some astronomers use the term QSO for this object reserving 'quasar' for radio-loud objects, while others use the terminology radio-quiet and radio-lo ...
The role of tidal interactions in star formation
... flows in many types of binary systems containing circumstellar discs (Matsuda et al. 2000; Menou 2000). The simulations mentioned above have all assumed nearly circular orbits for the stars, but tidal effects may be even more important in the more typical case of eccentric binaries, as the two stars ...
... flows in many types of binary systems containing circumstellar discs (Matsuda et al. 2000; Menou 2000). The simulations mentioned above have all assumed nearly circular orbits for the stars, but tidal effects may be even more important in the more typical case of eccentric binaries, as the two stars ...
Edmund C. Stoner and the discovery of the maximum mass of white
... pressure of the electrons caused by the exclusion principle. Fowler, however, did not attempt to determine the equilibrium properties of such a star which he regarded as “strictly analogous to one giant molecule in the ground state''. Apparently he was unaware that at the time, Llewellyn H. Thomas h ...
... pressure of the electrons caused by the exclusion principle. Fowler, however, did not attempt to determine the equilibrium properties of such a star which he regarded as “strictly analogous to one giant molecule in the ground state''. Apparently he was unaware that at the time, Llewellyn H. Thomas h ...
Characterizing the Cool KOIs III. KOI
... count for discrepancies between measured and predicted radii (e.g. Torres 2007). Unfortunately, KOI 961 does not have a parallax measurement in the literature, which is necessary to estimate its luminosity and hence mass. In a previous paper (Muirhead et al. 2011b, hereafter Paper 1), we acquired a ...
... count for discrepancies between measured and predicted radii (e.g. Torres 2007). Unfortunately, KOI 961 does not have a parallax measurement in the literature, which is necessary to estimate its luminosity and hence mass. In a previous paper (Muirhead et al. 2011b, hereafter Paper 1), we acquired a ...
How plausible are the proposed formation scenarios of CEMP
... Galaxy are also enriched in barium, whose solar-system abundance is mostly produced by the s-process (≈ 89%, Bisterzo et al. 2011), and are therefore called CEMP-s stars. To explain the simultaneous enrichments in carbon, barium, and other selements it has been suggested that CEMP-s stars underwent ...
... Galaxy are also enriched in barium, whose solar-system abundance is mostly produced by the s-process (≈ 89%, Bisterzo et al. 2011), and are therefore called CEMP-s stars. To explain the simultaneous enrichments in carbon, barium, and other selements it has been suggested that CEMP-s stars underwent ...
The formation of carbon dioxide in molecular
... be responsible for the large abundance of CO2 in a CO-rich ice, occurring after CO freeze-out onto the grain surface at AV ∼ 7 (Pontoppidan et al. 2003). A third epoch of CO2 formation, responsible for the high CO2 abundances towards YSOs and protostars, is likely to be CO2 formed in H2 O-dominated ...
... be responsible for the large abundance of CO2 in a CO-rich ice, occurring after CO freeze-out onto the grain surface at AV ∼ 7 (Pontoppidan et al. 2003). A third epoch of CO2 formation, responsible for the high CO2 abundances towards YSOs and protostars, is likely to be CO2 formed in H2 O-dominated ...
Direct Detection of Classically Undetectable Dark
... As universe expands, density of dark matter drops low enough that interactions become rare Dark matter streams around and clumps into galaxies today ...
... As universe expands, density of dark matter drops low enough that interactions become rare Dark matter streams around and clumps into galaxies today ...
The masses and spins of neutron stars and stellar
... As the remnants of core-collapse supernovae, neutron stars and black holes are also windows into the collapse and explosion processes. The further evolution of these systems in accreting binaries can tell us about the accretion process, e.g., the total amount of mass that is typically deposited on t ...
... As the remnants of core-collapse supernovae, neutron stars and black holes are also windows into the collapse and explosion processes. The further evolution of these systems in accreting binaries can tell us about the accretion process, e.g., the total amount of mass that is typically deposited on t ...
Shock interactions, turbulence and the origin of the stellar mass
... Galactic Plane Survey [14]. These 21 cm maps of radio emission show that the diffuse ISM is highly filamentary, and abounds in bubbles, cavities and channels carved out by radiation, winds and supernova explosions from massive stars. Most stars form in star clusters, and it is the massive stars with ...
... Galactic Plane Survey [14]. These 21 cm maps of radio emission show that the diffuse ISM is highly filamentary, and abounds in bubbles, cavities and channels carved out by radiation, winds and supernova explosions from massive stars. Most stars form in star clusters, and it is the massive stars with ...
Radial velocity planet detection biases at the stellar rotational period
... using the approximate prescription given by Aigrain et al. (2012), which yielded semi-amplitudes typically between 2 and 15 m s−1 , which are typical of active stars with high-amplitude photometric variability like those we have selected. We note that plages and faculae, which may cause significant ...
... using the approximate prescription given by Aigrain et al. (2012), which yielded semi-amplitudes typically between 2 and 15 m s−1 , which are typical of active stars with high-amplitude photometric variability like those we have selected. We note that plages and faculae, which may cause significant ...
the harps-terra project. i. description of the algorithms, performance
... The data analysis method required to extract such precise measurements consists of forward-modeling the spectrum of iodine multiplied by a high signal-to-noise ratio (S/N) template of the star and convolving the product with a parameterized model of the instrumental profile. This method was pioneere ...
... The data analysis method required to extract such precise measurements consists of forward-modeling the spectrum of iodine multiplied by a high signal-to-noise ratio (S/N) template of the star and convolving the product with a parameterized model of the instrumental profile. This method was pioneere ...
Power Point Presentation
... Pay attention to the lightcurves, optical counterparts and other properties of the bursts given on the reverse of the cards How many different types of bursts are there? Sort the bursts into different classes Fill out the accompanying worksheet to explain the reasoning behind your ...
... Pay attention to the lightcurves, optical counterparts and other properties of the bursts given on the reverse of the cards How many different types of bursts are there? Sort the bursts into different classes Fill out the accompanying worksheet to explain the reasoning behind your ...
P-nuclei
p-Nuclei (p stands for proton-rich) are certain proton-rich, naturally occurring isotopes of some elements between selenium and mercury which cannot be produced in either s- or r-process.