Roche accretion of stars close to massive black holes
... formed where the stream hits the disc. In addition, it is quite possible that one or two spiral arm shock waves will be created in the disc. The hotspot and shocks will orbit the hole with the orbital frequency of the star, and an inclined observer should see a modulation of the radiation from the d ...
... formed where the stream hits the disc. In addition, it is quite possible that one or two spiral arm shock waves will be created in the disc. The hotspot and shocks will orbit the hole with the orbital frequency of the star, and an inclined observer should see a modulation of the radiation from the d ...
Star formation bursts in isolated spiral galaxies
... fig. 2 of Sellwood and Carlberg (1984). In this simulation the stellar velocity dispersion is allowed to rise due to heating of the disc by gravitational instabilities. After several rotation periods, the rising velocity dispersion stabilizes the disc against non-axisymmetric instability, and the To ...
... fig. 2 of Sellwood and Carlberg (1984). In this simulation the stellar velocity dispersion is allowed to rise due to heating of the disc by gravitational instabilities. After several rotation periods, the rising velocity dispersion stabilizes the disc against non-axisymmetric instability, and the To ...
Cluster formation in molecular clouds – I. Stellar populations, star
... across large regions of the cloud (Megeath et al. 2012) so that the formation of a cluster would involve the eventual merger of a significant number of subclusters. There are several mechanisms that have been suggested as being responsible for shutting off accretion on to protostars and dispersing t ...
... across large regions of the cloud (Megeath et al. 2012) so that the formation of a cluster would involve the eventual merger of a significant number of subclusters. There are several mechanisms that have been suggested as being responsible for shutting off accretion on to protostars and dispersing t ...
Reconstructing the evolution of double helium white dwarfs
... cannot be excluded a priori. However, as we show in an forthcoming paper (Nelemans et al. 2000), in the majority of binary white dwarfs we indeed observe the youngest of the two dwarfs. From Figs. 1 and 2 we see that we find a range of Pm ’s and αλ’s for WD 0957-666, 1101+364 and 0136+768 where the m ...
... cannot be excluded a priori. However, as we show in an forthcoming paper (Nelemans et al. 2000), in the majority of binary white dwarfs we indeed observe the youngest of the two dwarfs. From Figs. 1 and 2 we see that we find a range of Pm ’s and αλ’s for WD 0957-666, 1101+364 and 0136+768 where the m ...
Advanced Topics in Cosmology: A Pedagogical Introduction
... baryons and their strong interaction is significant and somewhat difficult to model. We can ignore such complications at lower temperatures and — as we shall see — several interesting physical phenomena did take place during the later epochs with T . 1012 . The first thing we need to do is to determ ...
... baryons and their strong interaction is significant and somewhat difficult to model. We can ignore such complications at lower temperatures and — as we shall see — several interesting physical phenomena did take place during the later epochs with T . 1012 . The first thing we need to do is to determ ...
Estudio de la tasa de reacción 30P(alfa, p)33S de interés as
... Type I X-ray bursts are thermonuclear explosions which take place in binary systems, pairs of bound stars that orbit around a common center of gravity. X-ray binaries are among the brightest extra-solar objects and constitute the brightest class of X-ray sources in the sky. They are characterized by ...
... Type I X-ray bursts are thermonuclear explosions which take place in binary systems, pairs of bound stars that orbit around a common center of gravity. X-ray binaries are among the brightest extra-solar objects and constitute the brightest class of X-ray sources in the sky. They are characterized by ...
Vicky Kaspi Chandra Anomalous X-ray Pulsars Fotis Gavriil
... • SGRs (5): giant flares, short bursts, spectral changes, pulse profile changes, timing anomalies… • AXPs (9): short bursts, outbursts, slow flux changes, long-lived flares, glitches… – Most recognized only since 2002 ...
... • SGRs (5): giant flares, short bursts, spectral changes, pulse profile changes, timing anomalies… • AXPs (9): short bursts, outbursts, slow flux changes, long-lived flares, glitches… – Most recognized only since 2002 ...
Modeling the chemical evolution of the Galaxy halo
... unraveling the origin of halo stars through a detailed analysis of their chemical abundances revealed the existence of two distinct halo populations with a systematic difference in [α/Fe], [Cu/Fe], [Zn/Fe] and [Ba/Y], but not in [Mn/Fe], at a given metallicity (Nissen & Schuster 2010, 2011, and refer ...
... unraveling the origin of halo stars through a detailed analysis of their chemical abundances revealed the existence of two distinct halo populations with a systematic difference in [α/Fe], [Cu/Fe], [Zn/Fe] and [Ba/Y], but not in [Mn/Fe], at a given metallicity (Nissen & Schuster 2010, 2011, and refer ...
Separating gas-giant and ice-giant planets by halting pebble accretion
... In this work, we use surface densities in pebbles comparable to MMSN estimates, unless mentioned otherwise. This approximation is supported by theoretical models of protoplanetary discs that include dust growth by coagulation and radial drift of particles (Brauer et al. 2008; Birnstiel et al. 2012). ...
... In this work, we use surface densities in pebbles comparable to MMSN estimates, unless mentioned otherwise. This approximation is supported by theoretical models of protoplanetary discs that include dust growth by coagulation and radial drift of particles (Brauer et al. 2008; Birnstiel et al. 2012). ...
Letter to the Editor - Max-Planck
... Beaming immediately suggests a connection with the model presented above of nonthermal ECS from a relativistic jet in a microquasar. The peak luminosity of ECS appears amplified due to Doppler boosting by a factor of D5 for a continuous jet. Even using the mildly relativistic jet parameters appropri ...
... Beaming immediately suggests a connection with the model presented above of nonthermal ECS from a relativistic jet in a microquasar. The peak luminosity of ECS appears amplified due to Doppler boosting by a factor of D5 for a continuous jet. Even using the mildly relativistic jet parameters appropri ...
10) Physics and Chemistry of the Diffuse Interstellar Medium
... With the canonical value for the Cosmic Ray Ionization Rate Of ≈ 10-17 s-1 and a fast DR process, H3+ should not be observable in the diffuse ISM! ...
... With the canonical value for the Cosmic Ray Ionization Rate Of ≈ 10-17 s-1 and a fast DR process, H3+ should not be observable in the diffuse ISM! ...
WSokolov-PROTVINO
... with the associated models by Robertson et al. (2010, blue hatched region). The black lines in panel c show the stellar mass density ρstar implied by parameterizations of the GRB-derived star formation rate, which clearly exceed the stellar mass density ρstar at all redshifts. ...
... with the associated models by Robertson et al. (2010, blue hatched region). The black lines in panel c show the stellar mass density ρstar implied by parameterizations of the GRB-derived star formation rate, which clearly exceed the stellar mass density ρstar at all redshifts. ...
disks surviving the radiation pressure of radio pulsars
... kinetic energy density of the disk. Inside the light cylinder, the near zone electromagnetic field is essentially the dipole magnetic field, and the inner radius is the conventional Alfvén radius. Far outside the light cylinder, in the radiation zone, jEj ¼ jBj, and the electromagnetic energy densi ...
... kinetic energy density of the disk. Inside the light cylinder, the near zone electromagnetic field is essentially the dipole magnetic field, and the inner radius is the conventional Alfvén radius. Far outside the light cylinder, in the radiation zone, jEj ¼ jBj, and the electromagnetic energy densi ...