On the composition of GRBs` Collapsar jets
... ≤95 per cent (2σ ).5 The best-fitting plateaus extend from 5 to 25 s in the BATSE data (7.19/4 χ 2 /DOF), from 2.5 to 17 s in the FermiGBM data (10/5 χ 2 /DOF) and from 1 to 20 s in the Swift data (15.85/9 χ 2 /DOF). We account for three free parameters in our fit: the height of the plateau and the ...
... ≤95 per cent (2σ ).5 The best-fitting plateaus extend from 5 to 25 s in the BATSE data (7.19/4 χ 2 /DOF), from 2.5 to 17 s in the FermiGBM data (10/5 χ 2 /DOF) and from 1 to 20 s in the Swift data (15.85/9 χ 2 /DOF). We account for three free parameters in our fit: the height of the plateau and the ...
The Habitability of Proxima Centauri b I: Evolutionary Scenarios
... & Magain (1997) because they were too different from the other 5 they considered. Hinkel & Kane (2013) found the mean metallicity [Fe/H] of each of the two stars to be +0.28 and +0.31 and with a large spread of 0.16 and 0.11, respectively. While it is frustrating that different groups have arrived a ...
... & Magain (1997) because they were too different from the other 5 they considered. Hinkel & Kane (2013) found the mean metallicity [Fe/H] of each of the two stars to be +0.28 and +0.31 and with a large spread of 0.16 and 0.11, respectively. While it is frustrating that different groups have arrived a ...
Evolution of the atomic and molecular gas content of galaxies
... et al. (2010, 2012) modeled the partitioning of gas into Hi and H2 in radial bins in each galaxy, using both the metallicity-dependent recipes of Krumholz, McKee & Tumlinson (2009, hereafter KMT) and the pressure-based recipe of BR, and self-consistently implemented a H2 -based star formation recipe ...
... et al. (2010, 2012) modeled the partitioning of gas into Hi and H2 in radial bins in each galaxy, using both the metallicity-dependent recipes of Krumholz, McKee & Tumlinson (2009, hereafter KMT) and the pressure-based recipe of BR, and self-consistently implemented a H2 -based star formation recipe ...
- Spiral - Imperial College London
... with solar activity (see e.g. Fröhlich 2006; Ball et al. 2012; Solanki et al. 2013, and references therein), the regime of the solar variability in the visible part of the spectrum is still under debate. The Sun is located so close to the threshold between direct and inverse correlations of visible ...
... with solar activity (see e.g. Fröhlich 2006; Ball et al. 2012; Solanki et al. 2013, and references therein), the regime of the solar variability in the visible part of the spectrum is still under debate. The Sun is located so close to the threshold between direct and inverse correlations of visible ...
Building galaxies Hunt, Leslie Kipp
... that atomic gas mass fraction also varies along the Hubble sequence. On the other hand, the massto-light ratio measured in the B band remains relatively constant with morphology, even toward the very late spiral types (although see Burstein 1982). With data from Roberts & Haynes (1994), Figure 3 sho ...
... that atomic gas mass fraction also varies along the Hubble sequence. On the other hand, the massto-light ratio measured in the B band remains relatively constant with morphology, even toward the very late spiral types (although see Burstein 1982). With data from Roberts & Haynes (1994), Figure 3 sho ...
Evolution of the Milky Way with radial motions of stars and gas
... such coefficients from the simulation of an early-type barred disk and, applying them in a semi-analytical model of that same disk, they showed that all the main features of the N-body+SPH simulation can be reproduced to a good accuracy. They also showed that radial migration moves around not only “pa ...
... such coefficients from the simulation of an early-type barred disk and, applying them in a semi-analytical model of that same disk, they showed that all the main features of the N-body+SPH simulation can be reproduced to a good accuracy. They also showed that radial migration moves around not only “pa ...
Evolution of the atomic and molecular gas content of galaxies
... make predictions for the multi-phase gas content of galaxies. Obreschkow et al. (2009a) applied an empirical pressurebased recipe based on the results of Blitz & Rosolowsky (2006, hereafter BR) in post-processing to compute the Hi and H2 content of galaxies in the Millennium simulations (De Lucia & ...
... make predictions for the multi-phase gas content of galaxies. Obreschkow et al. (2009a) applied an empirical pressurebased recipe based on the results of Blitz & Rosolowsky (2006, hereafter BR) in post-processing to compute the Hi and H2 content of galaxies in the Millennium simulations (De Lucia & ...
Hint of a transiting extended atmosphere on 55 Cancri b⋆
... parameters into account. These choices are (i) the transit start (T b ) and end (T b ) times; and (ii) the wavelength domain in the Lyα line. The FAP associated with (i) is calculated with a boot-strap method, randomising the choices of T b and T b . In each trial, the transit depth is estimat ...
... parameters into account. These choices are (i) the transit start (T b ) and end (T b ) times; and (ii) the wavelength domain in the Lyα line. The FAP associated with (i) is calculated with a boot-strap method, randomising the choices of T b and T b . In each trial, the transit depth is estimat ...
Dawes Review. The tidal downsizing hypothesis of planet formation
... . 5 M⊕ , that is in between the terrestrial planet mass and the more distant ”ice giants” (such a core mass is allowed by the Jupiter’s interior models, e.g., Guillot, 2005), then Jupiter was not strongly affected by the feedback from its core. It is therefore reasonable that Jupiter kept all or a m ...
... . 5 M⊕ , that is in between the terrestrial planet mass and the more distant ”ice giants” (such a core mass is allowed by the Jupiter’s interior models, e.g., Guillot, 2005), then Jupiter was not strongly affected by the feedback from its core. It is therefore reasonable that Jupiter kept all or a m ...
Paper by Bessell, Castelli and Plez on Model atmospheres
... sect. 2. The colors in the present paper essentially supersede those of Wood & Bessell (1994). In the 1993 flux data there was evidence of some discontinuities in the computed colors of A-G stars. Castelli (1996) explained how to eliminate these discontinuities which were related to a modification o ...
... sect. 2. The colors in the present paper essentially supersede those of Wood & Bessell (1994). In the 1993 flux data there was evidence of some discontinuities in the computed colors of A-G stars. Castelli (1996) explained how to eliminate these discontinuities which were related to a modification o ...
The Multitude of Molecular Hydrogen Knots in the Helix Nebula 1
... of cometary knots that appear clearly in H2 emission. The H2 knots must lie in front of some highly ionized gas emitting in order to cause the extinction of the [OIII] emission. The fact that most of the H2 knots do not appear as [OIII] shadows indicates that most of the H2 knots are confined within ...
... of cometary knots that appear clearly in H2 emission. The H2 knots must lie in front of some highly ionized gas emitting in order to cause the extinction of the [OIII] emission. The fact that most of the H2 knots do not appear as [OIII] shadows indicates that most of the H2 knots are confined within ...
1 Discovery of peculiar periodic spectral
... ABSTRACT A Fourier transform analysis of 2.5 million spectra in the Sloan Digital Sky Survey was carried out to detect periodic spectral modulations. Signals having the same period were found in only 234 stars overwhelmingly in the F2 to K1 spectral range. The signals cannot be caused by instrument ...
... ABSTRACT A Fourier transform analysis of 2.5 million spectra in the Sloan Digital Sky Survey was carried out to detect periodic spectral modulations. Signals having the same period were found in only 234 stars overwhelmingly in the F2 to K1 spectral range. The signals cannot be caused by instrument ...
thick disk - asteroSTEP
... • In our Galaxy, the thick disk is old, and kinematically and chemically distinct from the thin disk. What does it represent in the galaxy formation process ? • The orbital eccentricity distribution will provide some guidance. • Chemical tagging will show if the thick disk formed as a small number o ...
... • In our Galaxy, the thick disk is old, and kinematically and chemically distinct from the thin disk. What does it represent in the galaxy formation process ? • The orbital eccentricity distribution will provide some guidance. • Chemical tagging will show if the thick disk formed as a small number o ...
3. The MONS Telescope requirements
... turn sets a requirement on the minimum length of the telescope tube. For scientific reasons (to allow access to all primary targets during the mission), we will need to observe down to 30 degrees from the limb of the Earth. With a 32 cm telescope we therefore need a tube length of at least 48 cm. Fo ...
... turn sets a requirement on the minimum length of the telescope tube. For scientific reasons (to allow access to all primary targets during the mission), we will need to observe down to 30 degrees from the limb of the Earth. With a 32 cm telescope we therefore need a tube length of at least 48 cm. Fo ...
Confirmation of Hostless Type Ia Supernovae Using Hubble Space
... We present deep Hubble Space Telescope imaging at the locations of four, potentially hostless, long-faded Type Ia supernovae (SNe Ia) in low-redshift, rich galaxy clusters that were identified in the Multi-Epoch Nearby Cluster Survey. Assuming a steep faint-end slope for the galaxy cluster luminosit ...
... We present deep Hubble Space Telescope imaging at the locations of four, potentially hostless, long-faded Type Ia supernovae (SNe Ia) in low-redshift, rich galaxy clusters that were identified in the Multi-Epoch Nearby Cluster Survey. Assuming a steep faint-end slope for the galaxy cluster luminosit ...
Multiwavelength observations of XTE J1118+480`s outburst
... 85% of sources are highly absorbed (X-ray observations): column density NH>1023 cm-2 X-ray absorption >> IR => absorbing matter local to neutron star ...
... 85% of sources are highly absorbed (X-ray observations): column density NH>1023 cm-2 X-ray absorption >> IR => absorbing matter local to neutron star ...
INSTRUCTION MANUAL
... sophisticated and easy to use telescopes available on the market today. Take time to read through this manual before embarking on your journey through the Universe. It may take a few observing sessions to become familiar with your NexStar, so you should keep this manual handy until you have fully ma ...
... sophisticated and easy to use telescopes available on the market today. Take time to read through this manual before embarking on your journey through the Universe. It may take a few observing sessions to become familiar with your NexStar, so you should keep this manual handy until you have fully ma ...
Downloaded - Royal Society Open Science
... high enough to burn helium. For stars with M flashes’. This value of 2.0 M represents a key transition mass; the duration and character of the mass loss changes markedly when crossing this threshold. After the core helium is exhausted, a heliumburning shell is formed. At this point, the star is sa ...
... high enough to burn helium. For stars with M flashes’. This value of 2.0 M represents a key transition mass; the duration and character of the mass loss changes markedly when crossing this threshold. After the core helium is exhausted, a heliumburning shell is formed. At this point, the star is sa ...
PDF file of document - University of Iowa Astrophysics
... commonly used in all sciences to express mass (kilograms, kg), size (meters, m), and time (seconds, s). It Stars, Galaxies and the Universe ...
... commonly used in all sciences to express mass (kilograms, kg), size (meters, m), and time (seconds, s). It Stars, Galaxies and the Universe ...
R136a1
RMC 136a1 (usually abbreviated to R136a1) is a Wolf-Rayet star located at the center of R136, the central condensation of stars of the large NGC 2070 open cluster in the Tarantula Nebula. It lies at a distance of about 50 kiloparsecs (163,000 light-years) in the Large Magellanic Cloud. It has the highest mass and luminosity of any known star, at 265 M☉ and 8.7 million L☉, and also one of the hottest at over 50,000 K.