The physics of neutron stars
... is comparable to Earth’s radius but almost 1000 times greater than the radius of a neutron star [3]. Therefore, the matter density in their interiors is less than one-thousandth of ρ0 . On the other hand, according to theoretical models, quark stars at M ∼ M⊙ may be even more compact than neutron st ...
... is comparable to Earth’s radius but almost 1000 times greater than the radius of a neutron star [3]. Therefore, the matter density in their interiors is less than one-thousandth of ρ0 . On the other hand, according to theoretical models, quark stars at M ∼ M⊙ may be even more compact than neutron st ...
An atlas of 2.4 to 4.1 mu m ISO/SWS spectra of early - UvA-DARE
... four preset overlapping sub-bands. These are defined in Table 4. The integration time per target is fixed, therefore the S/N ratio mainly depends on the brightness of the source. Combining the nominal and Post-Helium program AOT01 speed 4 observations, we collected 69 ISO/SWS spectra. However, two t ...
... four preset overlapping sub-bands. These are defined in Table 4. The integration time per target is fixed, therefore the S/N ratio mainly depends on the brightness of the source. Combining the nominal and Post-Helium program AOT01 speed 4 observations, we collected 69 ISO/SWS spectra. However, two t ...
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... since stars at the extremes of this distribution will follow very different post-main sequence evolutionary paths. Indeed, the inclusion of sgB[e] stars in such schemes is highly uncertain at present (Aret et al. 2012). Despite their co-location in the Hertzsprung-Russell (HR) diagram (cf. Clark et ...
... since stars at the extremes of this distribution will follow very different post-main sequence evolutionary paths. Indeed, the inclusion of sgB[e] stars in such schemes is highly uncertain at present (Aret et al. 2012). Despite their co-location in the Hertzsprung-Russell (HR) diagram (cf. Clark et ...
The (galaxy-wide) IMF in giant elliptical galaxies: from top to bottom
... (Ceff = 20) and negligible outflows (Bout = 0). Fig. 2 shows the relationship between the SFR and the gas-phase metallicity – giving a direct estimate of the stellar metallicity distribution – assuming a time-independent IMF. Note that at the high values of μ needed by the line strength analysis of ...
... (Ceff = 20) and negligible outflows (Bout = 0). Fig. 2 shows the relationship between the SFR and the gas-phase metallicity – giving a direct estimate of the stellar metallicity distribution – assuming a time-independent IMF. Note that at the high values of μ needed by the line strength analysis of ...
The impact of surface temperature inhomogeneities on quiescent
... the effects of variations between hydrogen atmosphere models (Heinke et al. 2006; Haakonsen et al. 2012), distance errors (Heinke et al. 2006; Guillot et al. 2011, 2013; Heinke et al. 2014; Bogdanov et al. 2016), detector systematics (Heinke et al. 2006; Guillot et al. 2011; Heinke et al. 2014), and ...
... the effects of variations between hydrogen atmosphere models (Heinke et al. 2006; Haakonsen et al. 2012), distance errors (Heinke et al. 2006; Guillot et al. 2011, 2013; Heinke et al. 2014; Bogdanov et al. 2016), detector systematics (Heinke et al. 2006; Guillot et al. 2011; Heinke et al. 2014), and ...
THE ORION NEBULA AND ITS ASSOCIATED POPULATION C. R. O
... was inconsistent with a spherically symmetric nebula and was used independently and essentially simultaneously by Balick et al. (1974) and Zuckerman (1973) to come up with today’s model. In a simple manner, the assumption of a thin emitting layer of radially decreasing density lying beyond the ioniz ...
... was inconsistent with a spherically symmetric nebula and was used independently and essentially simultaneously by Balick et al. (1974) and Zuckerman (1973) to come up with today’s model. In a simple manner, the assumption of a thin emitting layer of radially decreasing density lying beyond the ioniz ...
The rebirth of Supernova 1987A a study of the ejecta-ring collision
... At this mass, electron degeneracy pressure can no longer withstand the gravitational forces and, as a consequence, the iron core starts to contract. Due to electron captures in the iron core, e− + p → n + νe , the number of electrons decreases and the pressure reduces accordingly. Furthermore, energ ...
... At this mass, electron degeneracy pressure can no longer withstand the gravitational forces and, as a consequence, the iron core starts to contract. Due to electron captures in the iron core, e− + p → n + νe , the number of electrons decreases and the pressure reduces accordingly. Furthermore, energ ...
Stars as cosmological tools: giving light to Dark Matter
... One of the more tantalizing mysteries in modern science is the evidence that 83% of all the matter in the Universe exists in an undiscovered form, known as Dark Matter (DM), dierent from any other type of matter. Despite the extensive eorts dedicated to investigate the DM problem, the identi catio ...
... One of the more tantalizing mysteries in modern science is the evidence that 83% of all the matter in the Universe exists in an undiscovered form, known as Dark Matter (DM), dierent from any other type of matter. Despite the extensive eorts dedicated to investigate the DM problem, the identi catio ...
WSokolov-PROTVINO
... Gamma-ray bursts belong to the most distant observable objects with measurable redshift. Gamma-ray bursts are related to the star formation in distant (and very distant) galaxies. Gamma-ray bursts and their afterglows also allow us seeing the most distant explosions of massive stars at the end of th ...
... Gamma-ray bursts belong to the most distant observable objects with measurable redshift. Gamma-ray bursts are related to the star formation in distant (and very distant) galaxies. Gamma-ray bursts and their afterglows also allow us seeing the most distant explosions of massive stars at the end of th ...
INFRARED DUST BUBBLES: PROBING THE DETAILED
... to turbulent mixing. The consequence of this is that clumps of cool 104 K gas are predicted to be found mixed with the hot 107 K gas. The thickness of the 104 K shell is predicted to be a function both of age and luminosity of the central star; the lower the wind luminosity, the thicker the cool ion ...
... to turbulent mixing. The consequence of this is that clumps of cool 104 K gas are predicted to be found mixed with the hot 107 K gas. The thickness of the 104 K shell is predicted to be a function both of age and luminosity of the central star; the lower the wind luminosity, the thicker the cool ion ...
Period-Luminosity Relations for delta Scuti Stars
... at visible bands: the amplitude of the variables is smaller, with which the mean magnitudes have lower dispersion; the interstellar extinction is lower (AK /AV ∼ 1/10); and the infrared luminosities are less sensitive to temperature changes (instability strip is narrower), so PL relations are tighte ...
... at visible bands: the amplitude of the variables is smaller, with which the mean magnitudes have lower dispersion; the interstellar extinction is lower (AK /AV ∼ 1/10); and the infrared luminosities are less sensitive to temperature changes (instability strip is narrower), so PL relations are tighte ...
Effects of color superconductivity on the nucleation of quark matter in
... where Nc is the number of virtual centers of droplet formation in the innermost region of the star. Following the simple estimate given in Iida & Sato (1998), we take Nc = 1048 . The uncertainty in the value of Nc is expected to be within one or two orders of magnitude. In any case, all the qualitat ...
... where Nc is the number of virtual centers of droplet formation in the innermost region of the star. Following the simple estimate given in Iida & Sato (1998), we take Nc = 1048 . The uncertainty in the value of Nc is expected to be within one or two orders of magnitude. In any case, all the qualitat ...
Triggered/sequential star formation? A multi
... Results. We show that the bubble is spatially associated with G18.93, located at a kinematic near distance of 3.6 kpc. The total gas mass of ∼870 M splits up into 6 sub-clumps, of which G18.93/m is the most massive with 280 M . The virial analysis shows that it may be gravitationally bound and has ...
... Results. We show that the bubble is spatially associated with G18.93, located at a kinematic near distance of 3.6 kpc. The total gas mass of ∼870 M splits up into 6 sub-clumps, of which G18.93/m is the most massive with 280 M . The virial analysis shows that it may be gravitationally bound and has ...
Chapter: The Evolution of Binary Systems
... the donor star has either been transferred to the companion or been lost from the system. The end product will be a hydrogen-exhausted helium star with at most a small hydrogen-rich envelope.3 Mass accretion will also change the structure of the accreting star. If it is still on the main sequence, t ...
... the donor star has either been transferred to the companion or been lost from the system. The end product will be a hydrogen-exhausted helium star with at most a small hydrogen-rich envelope.3 Mass accretion will also change the structure of the accreting star. If it is still on the main sequence, t ...
Astronomy Astrophysics Kuiper belts around nearby stars &
... submm and mm wavelengths 3% of the FEPS stars show evidence of continuum emission, with a suggested decrease in dust masses and/or changes in the grain properties for stellar ages of 10−30 Myr (Carpenter et al. 2005). An additional advantage in making observations in the submm region is that measure ...
... submm and mm wavelengths 3% of the FEPS stars show evidence of continuum emission, with a suggested decrease in dust masses and/or changes in the grain properties for stellar ages of 10−30 Myr (Carpenter et al. 2005). An additional advantage in making observations in the submm region is that measure ...
Hypervelocity Stars and the Galactic Center
... A massive black hole (MBH) will inevitably unbind stars from the Galaxy. Hills (1988) coined the term “hypervelocity star” (hereafter HVS) to describe a star ejected at ∼1000 km s−1 from a three-body interaction with a MBH. HVSs are a general consequence of MBHs in any galaxy (e.g. Sherwin et al. 20 ...
... A massive black hole (MBH) will inevitably unbind stars from the Galaxy. Hills (1988) coined the term “hypervelocity star” (hereafter HVS) to describe a star ejected at ∼1000 km s−1 from a three-body interaction with a MBH. HVSs are a general consequence of MBHs in any galaxy (e.g. Sherwin et al. 20 ...
Chapter 6 in the LSST Science Book
... ΛCDM hierarchy. In our Galaxy the most metal poor, and (plausibly) the oldest observed stars are distributed in a halo that extends beyond 25 kpc. Their spatial distribution, chemical composition and kinematics provide clues about the Milky Way’s early history, as well as its continued interaction w ...
... ΛCDM hierarchy. In our Galaxy the most metal poor, and (plausibly) the oldest observed stars are distributed in a halo that extends beyond 25 kpc. Their spatial distribution, chemical composition and kinematics provide clues about the Milky Way’s early history, as well as its continued interaction w ...
RADIO OBSERVATIONS RELATED TO STAR FORMATION P. G.
... procedure; we introduce the review of observations (Sect. II) by outlining a working hypothesis for the evolutionary sequence of Ο and Β stars. This sequence is based on radio and IR observations of the giant HII region W3 (reviewed by Mezger and Wink, 1974) and on model calculations of dust-filled ...
... procedure; we introduce the review of observations (Sect. II) by outlining a working hypothesis for the evolutionary sequence of Ο and Β stars. This sequence is based on radio and IR observations of the giant HII region W3 (reviewed by Mezger and Wink, 1974) and on model calculations of dust-filled ...
The Spitzer/GLIMPSE Surveys - UW-Madison Astronomy
... extended objects that were especially bright in the 4.5 μm band of the IRAC detectors. These objects have been referred to by the GLIMPSE team as “green fuzzies” or extended green objects (EGOs) because the 4.5 μm band is commonly coded as green in false color images consisting of IRAC 3.6 μm (blue) ...
... extended objects that were especially bright in the 4.5 μm band of the IRAC detectors. These objects have been referred to by the GLIMPSE team as “green fuzzies” or extended green objects (EGOs) because the 4.5 μm band is commonly coded as green in false color images consisting of IRAC 3.6 μm (blue) ...
observations and theory of star cluster formation
... Young stars form on a wide range of scales, producing aggregates and clusters with various degrees of gravitational self-binding. The loose aggregates have a hierarchical structure in both space and time that resembles interstellar turbulence, suggesting that these stars form in only a few turbulent ...
... Young stars form on a wide range of scales, producing aggregates and clusters with various degrees of gravitational self-binding. The loose aggregates have a hierarchical structure in both space and time that resembles interstellar turbulence, suggesting that these stars form in only a few turbulent ...
as a PDF
... the inferred circumstellar masses of dust and gas surrounding classical T-Tauri Stars (cTTSs), measured by millimeter continuum observations, preclude a simple spherical distribution of the circumstellar material about such stars (Rydgren et al. 1982). The mass involved would, if spherically distrib ...
... the inferred circumstellar masses of dust and gas surrounding classical T-Tauri Stars (cTTSs), measured by millimeter continuum observations, preclude a simple spherical distribution of the circumstellar material about such stars (Rydgren et al. 1982). The mass involved would, if spherically distrib ...
A FUSE Survey of Coronal Forbidden Lines in Late
... that active stars have larger coronal emission measures than inactive stars, that giant stars all have reasonably similar emission measure distributions, and that all dwarf stars also share similar emission measure distributions. Although we have chosen specific active stars to demonstrate this techn ...
... that active stars have larger coronal emission measures than inactive stars, that giant stars all have reasonably similar emission measure distributions, and that all dwarf stars also share similar emission measure distributions. Although we have chosen specific active stars to demonstrate this techn ...
Radiative hydrodynamics simulations of red supergiant stars. III
... to the total length of the Gaia mission. As seen in the Figure, for t < 22 yr, the random displacement is small and increases to a maximum value of 0.30 AU at t ∼ 23 yr. In relation with the astrometric implications of this photocentre displacement, which will be discussed in Sect. 4, it must be str ...
... to the total length of the Gaia mission. As seen in the Figure, for t < 22 yr, the random displacement is small and increases to a maximum value of 0.30 AU at t ∼ 23 yr. In relation with the astrometric implications of this photocentre displacement, which will be discussed in Sect. 4, it must be str ...
Debris discs around M stars: non-existence versus non
... (iii) Planetesimals: the radius r, radial velocity dispersion σr and mass density ρ of the planetesimal. The stellar luminosity is given by L? = 4πR?2 σSB T?4 where σSB is the Stefan-Boltzmann constant. We obtain the values of the stellar parameters from Table 1 of Kaltenegger & Traub (2009). We ass ...
... (iii) Planetesimals: the radius r, radial velocity dispersion σr and mass density ρ of the planetesimal. The stellar luminosity is given by L? = 4πR?2 σSB T?4 where σSB is the Stefan-Boltzmann constant. We obtain the values of the stellar parameters from Table 1 of Kaltenegger & Traub (2009). We ass ...
The First Galaxies: Assembly under Radiative Feedback from the
... The most massive of the simulated MW dark matter subhalos have progenitors with masses 108 − 1010 M⊙ at z & 6 (e.g., Boylan-Kolchin et al. 2012). This suggests an intimate relation with the first dwarf galaxies, and renders investigations into these objects a promising tool to understand the origin ...
... The most massive of the simulated MW dark matter subhalos have progenitors with masses 108 − 1010 M⊙ at z & 6 (e.g., Boylan-Kolchin et al. 2012). This suggests an intimate relation with the first dwarf galaxies, and renders investigations into these objects a promising tool to understand the origin ...