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Astronomy 112: The Physics of Stars Class 1 Notes
... calibrated off human senses, the system is, like human senses, logarithmic. Every five magnitudes corresponds to a change of a factor of 100 in brightness. In this class we will not make any further use of the magnitude system, and will instead discuss only fluxes from stars, which can be measured d ...
... calibrated off human senses, the system is, like human senses, logarithmic. Every five magnitudes corresponds to a change of a factor of 100 in brightness. In this class we will not make any further use of the magnitude system, and will instead discuss only fluxes from stars, which can be measured d ...
Multiple Jets from the High-Mass (Proto) stellar Cluster AFGL5142
... 1999). Thus, dust emission dominates the 1.3mm continuum flux of all the sources, and likely does so to wavelengths as long as ∼ 3 mm. Because of a lack of high resolution images at more than one wavelength, the emissivity index of the dust emission at each peak cannot be evaluated. Instead, we conv ...
... 1999). Thus, dust emission dominates the 1.3mm continuum flux of all the sources, and likely does so to wavelengths as long as ∼ 3 mm. Because of a lack of high resolution images at more than one wavelength, the emissivity index of the dust emission at each peak cannot be evaluated. Instead, we conv ...
The galaxy stellar mass function at 3.5 ≤z ≤ 7.5 in the CANDELS
... is steeper than has been found at lower redshifts, but appears to be unchanged over the redshift range probed here. Meanwhile the high-mass end of the GSMF appears to evolve primarily in density, although there is also some evidence of evolution in characteristic mass. Our results are very different ...
... is steeper than has been found at lower redshifts, but appears to be unchanged over the redshift range probed here. Meanwhile the high-mass end of the GSMF appears to evolve primarily in density, although there is also some evidence of evolution in characteristic mass. Our results are very different ...
2. The X-ray-Radio correlation for bulgeless galaxies
... Active Galactic Nuclei (AGN) and in Star Forming galaxies. For the first case, the Xray/Radio correlation seems to present different slopes for Radio-loud and Radio-quiet AGN and may be used to estimate the mass of the central black hole in these galaxies, while in the second case the correlation ap ...
... Active Galactic Nuclei (AGN) and in Star Forming galaxies. For the first case, the Xray/Radio correlation seems to present different slopes for Radio-loud and Radio-quiet AGN and may be used to estimate the mass of the central black hole in these galaxies, while in the second case the correlation ap ...
Circumstellar dust emission from nearby Solar
... which is a sign-post for extrasolar planets, and was first detected in the mid 1980s. Dust discs are intricately connected to planets and planetesimals, give insights in the dynamics and evolution of the system, and are also useful for future exoplanet-observations. This thesis is aimed at modelling ...
... which is a sign-post for extrasolar planets, and was first detected in the mid 1980s. Dust discs are intricately connected to planets and planetesimals, give insights in the dynamics and evolution of the system, and are also useful for future exoplanet-observations. This thesis is aimed at modelling ...
Strongly suggested reading: The Milky Way`s stellar disk
... three-dimensional gravitational potential and by implication the dark-matter distribution in the Milky Way. A sequence of ongoing photometry and spectroscopy surveys has recently hundred-folded the number of stars with good distances, radial and transverse velocities, and abundance estimates; this o ...
... three-dimensional gravitational potential and by implication the dark-matter distribution in the Milky Way. A sequence of ongoing photometry and spectroscopy surveys has recently hundred-folded the number of stars with good distances, radial and transverse velocities, and abundance estimates; this o ...
IRC −10414: a bow-shock-producing red supergiant star
... through the red supergiant (RSG) phase during their lifetimes. Nonetheless, although many dozens of massive runaways were found to be associated with bow shocks, only two RSG bow-shock-producing stars, Betelgeuse and μ Cep, are known to date. In this paper, we report the discovery of an arc-like neb ...
... through the red supergiant (RSG) phase during their lifetimes. Nonetheless, although many dozens of massive runaways were found to be associated with bow shocks, only two RSG bow-shock-producing stars, Betelgeuse and μ Cep, are known to date. In this paper, we report the discovery of an arc-like neb ...
Comparison between the luminosity functions of X
... for all sources with a reliable Seyfert classification. There are 38 sources in the sample, of which 30 are classified as type2 and eight as type-1. We correct the X-ray luminosities for absorption using the observed column densities given in that paper. There are five Seyfert-2 galaxies which do no ...
... for all sources with a reliable Seyfert classification. There are 38 sources in the sample, of which 30 are classified as type2 and eight as type-1. We correct the X-ray luminosities for absorption using the observed column densities given in that paper. There are five Seyfert-2 galaxies which do no ...
A Theory of Extrasolar Giant Planets
... with the latter playing no signi cant role in the interior structure. However, we also examine the eect of enhancing metals well above solar composition. Our theory does not include objects similar to the ice giant planets Uranus and Neptune. These belong to a dierent class of object because they ...
... with the latter playing no signi cant role in the interior structure. However, we also examine the eect of enhancing metals well above solar composition. Our theory does not include objects similar to the ice giant planets Uranus and Neptune. These belong to a dierent class of object because they ...
Protoplanetary Disks and their Evolution
... versus that accreted onto the protostar. The instabilities would lead to sporadic bursts of high accretion and effectively self-regulate the disk mass from growing faster than the star (Vorobyov & Basu 2005, 2006; Vorobyov 2010). Many protostars have been observed to undergo short-lived bursts of ac ...
... versus that accreted onto the protostar. The instabilities would lead to sporadic bursts of high accretion and effectively self-regulate the disk mass from growing faster than the star (Vorobyov & Basu 2005, 2006; Vorobyov 2010). Many protostars have been observed to undergo short-lived bursts of ac ...
variation in the pre-transit balmer line signal around
... handful of hot planet systems, namely, WASP-12 b (Fossati et al. 2010), HD 189733 b (Ben-Jaffel & Ballester 2013; Bourrier et al. 2013; Cauley et al. 2015), and GJ 436 b (Ehrenreich et al. 2015; see Section 1 of Cauley et al. 2015, for a brief overview). Most recently, Ehrenreich et al. (2015) repor ...
... handful of hot planet systems, namely, WASP-12 b (Fossati et al. 2010), HD 189733 b (Ben-Jaffel & Ballester 2013; Bourrier et al. 2013; Cauley et al. 2015), and GJ 436 b (Ehrenreich et al. 2015; see Section 1 of Cauley et al. 2015, for a brief overview). Most recently, Ehrenreich et al. (2015) repor ...
paper - Harvard-Smithsonian Center for Astrophysics
... four identified SO2 lines vary from 19 to 130 K. All four of these lines were detected in the spectral line survey of Tenenbaum et al. (2010). Our interferometric observations reveal the spatial distribution of the SO2 emission for the first time. The spectra and integrated maps of all four lines ar ...
... four identified SO2 lines vary from 19 to 130 K. All four of these lines were detected in the spectral line survey of Tenenbaum et al. (2010). Our interferometric observations reveal the spatial distribution of the SO2 emission for the first time. The spectra and integrated maps of all four lines ar ...
The Properties of Super Star Clusters in A Sample of
... people most likely to read them who most deserve to acknowledged, and I will undoubtedly realize as soon as this thesis has been printed that several important people have been inadvertently left out. My sincere apologies in advance — to everyone who has provided me with kind words, a welcome ear, n ...
... people most likely to read them who most deserve to acknowledged, and I will undoubtedly realize as soon as this thesis has been printed that several important people have been inadvertently left out. My sincere apologies in advance — to everyone who has provided me with kind words, a welcome ear, n ...
Gamma Ray Bursts
... Diversity of pulse shapes well explained by diversity of shapes and sizes of comets. Neutron stars are inside galactic disk. How to get isotropic distribution? Possible, if we see only nearby neutron stars. Having the number of neutron stars (from pulsar observations and supernovae) and the numer of ...
... Diversity of pulse shapes well explained by diversity of shapes and sizes of comets. Neutron stars are inside galactic disk. How to get isotropic distribution? Possible, if we see only nearby neutron stars. Having the number of neutron stars (from pulsar observations and supernovae) and the numer of ...
SN 2011dh and the progenitors of Type IIb supernovae Mattias Ergon
... Core-collapse supernovae (SNe) are the observed events following the collapse of the core of evolved massive stars. The gravitational energy released creates a powerful shock that disrupts the star and ejects the heated material into the surrounding circumstellar medium. The observed properties depe ...
... Core-collapse supernovae (SNe) are the observed events following the collapse of the core of evolved massive stars. The gravitational energy released creates a powerful shock that disrupts the star and ejects the heated material into the surrounding circumstellar medium. The observed properties depe ...
Three Binary Millisecond Pulsars in NGC 6266
... Their accelerations toward the cluster center yield values of the cluster central density and mass-to-light ratio consistent with those derived from optical data. The three pulsars are in binary systems. One (spin period P ¼ 5:24 ms) is in a 3.5 day orbit around a companion of minimum mass 0.2 M. T ...
... Their accelerations toward the cluster center yield values of the cluster central density and mass-to-light ratio consistent with those derived from optical data. The three pulsars are in binary systems. One (spin period P ¼ 5:24 ms) is in a 3.5 day orbit around a companion of minimum mass 0.2 M. T ...
Mid-IR Spectra of IRAS 20343+4129 IRS 1 and IRS 3 M.F. Campbell
... IRAS 20343+4129 was identified as a candidate high-mass protostellar object (HMPO) by Sridharan et al. (2002) It was mapped in 1.2 mm dust continuum emission by Beuther et al. (2002a) and found to have a pair of massive clumps oriented ~EW (contours in Fig 1., taken from Palau, 2006). Beuther et al. ...
... IRAS 20343+4129 was identified as a candidate high-mass protostellar object (HMPO) by Sridharan et al. (2002) It was mapped in 1.2 mm dust continuum emission by Beuther et al. (2002a) and found to have a pair of massive clumps oriented ~EW (contours in Fig 1., taken from Palau, 2006). Beuther et al. ...
The ATLAS3D Project – XXX. Star formation histories and stellar
... weaker iron, we use the fact that some galaxies have a measurable Fe5270 index, which is free from nebular emission contamination. Fig. 1 shows several galaxies where Fe5270 also lies below the general relation, but the ratio of the two iron indices (bottom panel of Fig. 1) is consistent with the sa ...
... weaker iron, we use the fact that some galaxies have a measurable Fe5270 index, which is free from nebular emission contamination. Fig. 1 shows several galaxies where Fe5270 also lies below the general relation, but the ratio of the two iron indices (bottom panel of Fig. 1) is consistent with the sa ...
CHARACTERIZING THE COOL KOIs. III. KOI 961: A SMALL STAR
... of low-mass KOIs. The spectrum confirmed that it is a dwarf and not a giant based on the shallowness of the CO absorption band, and we reported an effective temperature of 3200 ± 50 K and an overall metallicity ([M/H]) of −0.33 ± 0.12 using the spectroscopic indices and calibrations of Rojas-Ayala e ...
... of low-mass KOIs. The spectrum confirmed that it is a dwarf and not a giant based on the shallowness of the CO absorption band, and we reported an effective temperature of 3200 ± 50 K and an overall metallicity ([M/H]) of −0.33 ± 0.12 using the spectroscopic indices and calibrations of Rojas-Ayala e ...
H EMISSION FROM HIGH-VELOCITY CLOUDS AND
... having upper limits on the order of 30–70 mR. The H measurements are discussed in relation to their H i properties, and distance constraints are given to each of the complexes based on f^esc 6% of the ionizing photons escaping normal to the Galactic disk ( fesc 1% 2% when averaged over solid an ...
... having upper limits on the order of 30–70 mR. The H measurements are discussed in relation to their H i properties, and distance constraints are given to each of the complexes based on f^esc 6% of the ionizing photons escaping normal to the Galactic disk ( fesc 1% 2% when averaged over solid an ...
Neutron Stars in Compact Binary Systems: From the equation of
... the full set of Einstein equations by imposing an exact helical symmetry. However, we find that the helically-symmetric solution must be matched to a waveless boundary region to achieve convergence. Work with toy models suggests this lack of convergence is intractable, but the agreement of waveless ...
... the full set of Einstein equations by imposing an exact helical symmetry. However, we find that the helically-symmetric solution must be matched to a waveless boundary region to achieve convergence. Work with toy models suggests this lack of convergence is intractable, but the agreement of waveless ...
Multiplicity in Early Stellar Evolution
... Bonnell et al., 2008; Bate, 2009a,b; Attwood et al., 2009). 3D HD SPH calculations by Bate (2009a) made predictions of the frequency of single, binary, triple and quadruple star systems formed during the collapse of a highly unstable cloud with an initial mass of 500 M⊙ , a Jeans mass of 1 M⊙ , and ...
... Bonnell et al., 2008; Bate, 2009a,b; Attwood et al., 2009). 3D HD SPH calculations by Bate (2009a) made predictions of the frequency of single, binary, triple and quadruple star systems formed during the collapse of a highly unstable cloud with an initial mass of 500 M⊙ , a Jeans mass of 1 M⊙ , and ...
Cygnus X-1
Cygnus X-1 (abbreviated Cyg X-1) is a well-known galactic X-ray source, thought to be a black hole, in the constellation Cygnus. It was discovered in 1964 during a rocket flight and is one of the strongest X-ray sources seen from Earth, producing a peak X-ray flux density of 6977229999999999999♠2.3×10−23 Wm−2 Hz−1 (7003230000000000000♠2.3×103 Jansky). Cygnus X-1 was the first X-ray source widely accepted to be a black hole and it remains among the most studied astronomical objects in its class. The compact object is now estimated to have a mass about 14.8 times the mass of the Sun and has been shown to be too small to be any known kind of normal star, or other likely object besides a black hole. If so, the radius of its event horizon is about 7004440000000000000♠44 km.Cygnus X-1 belongs to a high-mass X-ray binary system about 7019574266339685654♠6070 ly from the Sun that includes a blue supergiant variable star designated HDE 226868 which it orbits at about 0.2 AU, or 20% of the distance from the Earth to the Sun. A stellar wind from the star provides material for an accretion disk around the X-ray source. Matter in the inner disk is heated to millions of degrees, generating the observed X-rays. A pair of jets, arranged perpendicular to the disk, are carrying part of the energy of the infalling material away into interstellar space.This system may belong to a stellar association called Cygnus OB3, which would mean that Cygnus X-1 is about five million years old and formed from a progenitor star that had more than 7001400000000000000♠40 solar masses. The majority of the star's mass was shed, most likely as a stellar wind. If this star had then exploded as a supernova, the resulting force would most likely have ejected the remnant from the system. Hence the star may have instead collapsed directly into a black hole.Cygnus X-1 was the subject of a friendly scientific wager between physicists Stephen Hawking and Kip Thorne in 1975, with Hawking betting that it was not a black hole. He conceded the bet in 1990 after observational data had strengthened the case that there was indeed a black hole in the system. This hypothesis has not been confirmed due to a lack of direct observation but has generally been accepted from indirect evidence.