arXiv:1410.8731v2 [astro
... We analyse and report in detail new near-infrared (1.45 - 2.45 microns) observations of the Dusty S-cluster Object (DSO/G2) during its approach to the black hole at the center of the Galaxy that were carried out with ESO VLT/SINFONI between February and September 2014. Before May 2014 we detect spat ...
... We analyse and report in detail new near-infrared (1.45 - 2.45 microns) observations of the Dusty S-cluster Object (DSO/G2) during its approach to the black hole at the center of the Galaxy that were carried out with ESO VLT/SINFONI between February and September 2014. Before May 2014 we detect spat ...
Th`ese d`astrophysique Chemodynamical Simulations of Evolution
... and in the interstellar medium, using both observations and results from semi-analytic models (eliminating few of their assumptions). Once my model was set up, I have performed simulations of a massive galaxy to understand local effects on dust evolution. Simulations of dwarf galaxies have been carr ...
... and in the interstellar medium, using both observations and results from semi-analytic models (eliminating few of their assumptions). Once my model was set up, I have performed simulations of a massive galaxy to understand local effects on dust evolution. Simulations of dwarf galaxies have been carr ...
The Evolution of Long-Period Comets
... to reconcile with theory. Among the discrepancies is the \fading problem": the fraction of comets in the observed sample which are presumed to have made more than one perihelion passage since leaving the Oort cloud is much smaller than that predicted by simple dynamical models of the Solar System. T ...
... to reconcile with theory. Among the discrepancies is the \fading problem": the fraction of comets in the observed sample which are presumed to have made more than one perihelion passage since leaving the Oort cloud is much smaller than that predicted by simple dynamical models of the Solar System. T ...
Dust attenuation up to z ≃ 2 in the AKARI North Ecliptic Pole Deep
... and within galaxies like the Milky Way, about half of the stellar light is absorbed and re-emitted by dust at wavelengths larger than ∼5 µm, and that fraction can increase to more than 90% in starbursting objects. Therefore measuring the IR emission of galaxies has been identified as mandatory for m ...
... and within galaxies like the Milky Way, about half of the stellar light is absorbed and re-emitted by dust at wavelengths larger than ∼5 µm, and that fraction can increase to more than 90% in starbursting objects. Therefore measuring the IR emission of galaxies has been identified as mandatory for m ...
From Filamentary Networks to Dense Cores in Molecular Clouds
... star clusters. Numerical simulations now successfully include turbulence, gravity, a variety of cooling processes, MHD, and most recently, radiation and radiative feedback from massive stars. These numerical advances have been essential in testing and developing new insights into the physics of fila ...
... star clusters. Numerical simulations now successfully include turbulence, gravity, a variety of cooling processes, MHD, and most recently, radiation and radiative feedback from massive stars. These numerical advances have been essential in testing and developing new insights into the physics of fila ...
MULTIFREQUENCY VLBI STUDIES OF COMPACT EXTRAGALACTIC JETS by
... Homan 2005, and Jorstad et al. 2005), multifrequency VLBI studies targeting to observe the continuum spectrum of the jets have been less numerous. However, VLBA’s capability to make practically simultaneous multifrequency observations allows one to make such spectral studies and to obtain important ...
... Homan 2005, and Jorstad et al. 2005), multifrequency VLBI studies targeting to observe the continuum spectrum of the jets have been less numerous. However, VLBA’s capability to make practically simultaneous multifrequency observations allows one to make such spectral studies and to obtain important ...
Oxygen, magnesium and chromium isotopic ratios of
... the grains come from red giant branch (RGB) or asymptotic giant branch (AGB) stars. With the NanoSIMS, we measured the magnesium isotopic compositions of all 30 grains. We also measured the Cr isotopic ratios of the three Orgueil grains and one OC grain. Two of the Orgueil grains are very rich in Cr ...
... the grains come from red giant branch (RGB) or asymptotic giant branch (AGB) stars. With the NanoSIMS, we measured the magnesium isotopic compositions of all 30 grains. We also measured the Cr isotopic ratios of the three Orgueil grains and one OC grain. Two of the Orgueil grains are very rich in Cr ...
The Mass of Quasars Yue Shen
... the Salpeter time or e-folding time. If quasars do not radiate beyond the Eddington limit λ = 1, the observed luminosity provides a lower-limit on their BH mass (e.g., Zel’dovich & Novikov 1964). The discovery of luminous quasars (with Lbol & 1047 erg s−1) at z > 6 (e.g., Fan et al. 2001; Mortlock e ...
... the Salpeter time or e-folding time. If quasars do not radiate beyond the Eddington limit λ = 1, the observed luminosity provides a lower-limit on their BH mass (e.g., Zel’dovich & Novikov 1964). The discovery of luminous quasars (with Lbol & 1047 erg s−1) at z > 6 (e.g., Fan et al. 2001; Mortlock e ...
Giant Molecular Clouds in Local Group Galaxies
... galaxies do not suffer from this problem and as can be seen in Figs. 1 – 4, the clouds are, in general, spatially well separated, ensuring that we are almost always seeing only a single GMC along the line of sight. One of the long debated questions related to GMCs is: how does metallicity affect the ...
... galaxies do not suffer from this problem and as can be seen in Figs. 1 – 4, the clouds are, in general, spatially well separated, ensuring that we are almost always seeing only a single GMC along the line of sight. One of the long debated questions related to GMCs is: how does metallicity affect the ...
PSRD: Chondrules: Important, but Possibly Unfathomable
... What is the relationship between chondrules and CAIs? CAIs formed earlier by 2–3 million years, suggesting a progression from melting refractory materials first, then the more abundant materials that make up chondrules. Was this progression due to the process that did the melting or to the environme ...
... What is the relationship between chondrules and CAIs? CAIs formed earlier by 2–3 million years, suggesting a progression from melting refractory materials first, then the more abundant materials that make up chondrules. Was this progression due to the process that did the melting or to the environme ...
Accretion Power in Astrophysics, Third Editiion
... sources of the stars are wholly inadequate. The extraction of gravitational potential energy from material which accretes on to a gravitating body is now known to be the principal source of power in several types of close binary systems, and is widely believed to provide the power supply in active g ...
... sources of the stars are wholly inadequate. The extraction of gravitational potential energy from material which accretes on to a gravitating body is now known to be the principal source of power in several types of close binary systems, and is widely believed to provide the power supply in active g ...
![arXiv:1601.01542v1 [astro-ph.GA] 7 Jan 2016](http://s1.studyres.com/store/data/017487687_1-243c4cbda96da53325dd347b0c588a3e-300x300.png)
arXiv:1601.01542v1 [astro-ph.GA] 7 Jan 2016
... new stars. The ISM is fundamentally gaseous, and its chemical abundance can be derived by analysing spectroscopic features, that is, nebular emission lines. These emission lines are excited by photoionisation of the interstellar gas by hot and young massive stars (Aller 1984; Osterbrock 1989), which ...
... new stars. The ISM is fundamentally gaseous, and its chemical abundance can be derived by analysing spectroscopic features, that is, nebular emission lines. These emission lines are excited by photoionisation of the interstellar gas by hot and young massive stars (Aller 1984; Osterbrock 1989), which ...
High-mass X-ray Binaries: X-raying the winds Ángel Giménez García
... XSPEC, versión 12.8.08 , especializado en el ajuste de modelos a espectros de rayos X. En la Tabla 4.2 presentamos todos los modelos del continuo que hemos probado en cada uno de los espectros analizados. Los modelos has sido aceptados o rechazados en función del χ2 -reducido asociado a cada ajuste ...
... XSPEC, versión 12.8.08 , especializado en el ajuste de modelos a espectros de rayos X. En la Tabla 4.2 presentamos todos los modelos del continuo que hemos probado en cada uno de los espectros analizados. Los modelos has sido aceptados o rechazados en función del χ2 -reducido asociado a cada ajuste ...
Testing the Initial-Final Mass Relationship of White Dwarfs Silvia Catal´ an Ruiz
... results of an observational campaign devoted to measure the spectroscopic properties of a handful of white dwarfs in non-interacting binaries and, more precisely, in common proper motion pairs. This allows a direct test of the initial-final mass relationship. For these systems it is sound to assume ...
... results of an observational campaign devoted to measure the spectroscopic properties of a handful of white dwarfs in non-interacting binaries and, more precisely, in common proper motion pairs. This allows a direct test of the initial-final mass relationship. For these systems it is sound to assume ...
The HNC/HCN Ratio in Star-Forming Regions The Harvard
... - 100 K). Prior to the analysis of the HNC/HCN results, the observed abundances of CO, NH3 , N2 H+ , and HCO+ in OMC -1 (Murata et al. 1990; Ungerechts et al. 1997) were compared with model results. Agreement within an order of magnitude generally occurs at times between 2 × 105 and 1 × 108 yrs and ...
... - 100 K). Prior to the analysis of the HNC/HCN results, the observed abundances of CO, NH3 , N2 H+ , and HCO+ in OMC -1 (Murata et al. 1990; Ungerechts et al. 1997) were compared with model results. Agreement within an order of magnitude generally occurs at times between 2 × 105 and 1 × 108 yrs and ...
Link - Max-Planck-Institut für Astronomie
... predictions of Kenyon and Hartmann, (1991) and Turner et al., (1997), except at wavelengths longward of 25 µm. 2.3.2. Variability and episodic accretion. In addition to broad lightcurve evolution, FUors exhibit a variety of shorttimescale (hours to days) variability, both semi-periodic and stochasti ...
... predictions of Kenyon and Hartmann, (1991) and Turner et al., (1997), except at wavelengths longward of 25 µm. 2.3.2. Variability and episodic accretion. In addition to broad lightcurve evolution, FUors exhibit a variety of shorttimescale (hours to days) variability, both semi-periodic and stochasti ...
Physics of Neutron Star Crusts
... is expected to be very different from that formed during the aftermath of a supernova explosion. We show how it can be a site for nuclear reactions. We study its thermal structure during accretion, and briefly review the phenomenon of X-ray bursts. We quantitatively analyze the phenomenon of deep cru ...
... is expected to be very different from that formed during the aftermath of a supernova explosion. We show how it can be a site for nuclear reactions. We study its thermal structure during accretion, and briefly review the phenomenon of X-ray bursts. We quantitatively analyze the phenomenon of deep cru ...
