KELT-7b: A HOT JUPITER TRANSITING A BRIGHT V = 8.54
... directly predicted by the rotation velocity measured from the spectrum, combined with the transit depth and shape. The RM effect can therefore provide strong confirmation that the transit signal is due to a planetary-sized object transiting the target star. However, for Jupiter-sized companions, this ...
... directly predicted by the rotation velocity measured from the spectrum, combined with the transit depth and shape. The RM effect can therefore provide strong confirmation that the transit signal is due to a planetary-sized object transiting the target star. However, for Jupiter-sized companions, this ...
This is the Title - Astronomy at Swarthmore College
... The circumstellar chemistry of asymptotic giant branch (AGB) stars is particularly interesting. Asymptotic giant branch stars are chemically active due to their high metallicity, which fosters the creation of complex molecules. Giants are at a point in their evolutionary track where they have burnt ...
... The circumstellar chemistry of asymptotic giant branch (AGB) stars is particularly interesting. Asymptotic giant branch stars are chemically active due to their high metallicity, which fosters the creation of complex molecules. Giants are at a point in their evolutionary track where they have burnt ...
Fe I/Fe II ionization equilibrium in cool stars: NLTE versus LTE
... The NLTE, SH = 0 and LTE abundances obtained from the lines of Fe I (denoted as [Fe/H]I ) and Fe II ([Fe/H]II ) are presented in Table 1. It is worth noting that, with the updated model atom of Fe I-II, the departures from LTE are substantially smaller compared to those from the previous studies. Fo ...
... The NLTE, SH = 0 and LTE abundances obtained from the lines of Fe I (denoted as [Fe/H]I ) and Fe II ([Fe/H]II ) are presented in Table 1. It is worth noting that, with the updated model atom of Fe I-II, the departures from LTE are substantially smaller compared to those from the previous studies. Fo ...
Detection of Planetary Emission from the Exoplanet TrES
... (Burrows et al. 2007b; Knutson et al. 2008), it is incomplete. The relatively lower insolation experienced by the planet XO-1b is similar to that of TrES-1, and hence both atmospheres would be predicted to have water absorption features, as is indeed supported by the infrared observations of TrES-1 ...
... (Burrows et al. 2007b; Knutson et al. 2008), it is incomplete. The relatively lower insolation experienced by the planet XO-1b is similar to that of TrES-1, and hence both atmospheres would be predicted to have water absorption features, as is indeed supported by the infrared observations of TrES-1 ...
Article PDF - IOPscience
... Although data on external galaxies are fewer and much less detailed, they have still allowed their study with the use of similar methods. However, the number of parameters involved in any chemical evolution model is large, and a unique solution to the problem does not exist. Even the evolutionary pi ...
... Although data on external galaxies are fewer and much less detailed, they have still allowed their study with the use of similar methods. However, the number of parameters involved in any chemical evolution model is large, and a unique solution to the problem does not exist. Even the evolutionary pi ...
Search for giant planets in M67 III: excess of Hot Jupiters in dense
... This target has been observed since January 2008: 19 RV points have been obtained with HARPS with a typical S/N of 15 (per pixel at 550 nm) and a mean measurement uncertainty of 15 m s−1 including calibration errors. Other 5 additional RV measurements were obtained with SOPHIE and 2 with HARPS-N wit ...
... This target has been observed since January 2008: 19 RV points have been obtained with HARPS with a typical S/N of 15 (per pixel at 550 nm) and a mean measurement uncertainty of 15 m s−1 including calibration errors. Other 5 additional RV measurements were obtained with SOPHIE and 2 with HARPS-N wit ...
Key paper.
... for dust grains in the interstellar medium (ISM). This could be due to a population of grains in the MWC480 disk that are larger than 1 mm in size17, that is, several orders of magnitude greater than the sizes of ISM grains. Although this raises the possibility of grain accumulation, perhaps associa ...
... for dust grains in the interstellar medium (ISM). This could be due to a population of grains in the MWC480 disk that are larger than 1 mm in size17, that is, several orders of magnitude greater than the sizes of ISM grains. Although this raises the possibility of grain accumulation, perhaps associa ...
Migrating planets and migrating theories
... Uranus and Neptune originally formed much closer to our sun than where they currently reside. Also, at one time Jupiter and Saturn supposedly had different orbits that nudged Uranus and Neptune just right to cause them to migrate outward from the sun. The model also proposes that matter left over af ...
... Uranus and Neptune originally formed much closer to our sun than where they currently reside. Also, at one time Jupiter and Saturn supposedly had different orbits that nudged Uranus and Neptune just right to cause them to migrate outward from the sun. The model also proposes that matter left over af ...
Circular Polarization in Star- Formation Regions
... Because of the high obscuration, these regions are directly observable only at IR and radio wavelengths, whereas the circular dichroism bands in amino acids and similar molecules are in the UV at wavelengths of about 200 to 250 nm. We therefore investigated whether the mechanism responsible for the ...
... Because of the high obscuration, these regions are directly observable only at IR and radio wavelengths, whereas the circular dichroism bands in amino acids and similar molecules are in the UV at wavelengths of about 200 to 250 nm. We therefore investigated whether the mechanism responsible for the ...
Fill in the blanks of each frame using the list of missing words given
... heat has all gone, it sits as a cold dark mass, called a Black Dwarf. ...
... heat has all gone, it sits as a cold dark mass, called a Black Dwarf. ...
Andromeda and the Local Group Lesson Plan
... Way, and we’ll take a closer look at some of the nebula inside galaxies that are orbiting our own. Show the video. Review what they saw: ...
... Way, and we’ll take a closer look at some of the nebula inside galaxies that are orbiting our own. Show the video. Review what they saw: ...
Expanding the Catalog: Considering the Importance
... for burning in the core. For our highest mass stars that develop convective cores the extent of the convective core changes slightly due to the change in electron fraction (the convective core is high enough in temperature to be dominated by electron scattering opacity) and the energy generation by ...
... for burning in the core. For our highest mass stars that develop convective cores the extent of the convective core changes slightly due to the change in electron fraction (the convective core is high enough in temperature to be dominated by electron scattering opacity) and the energy generation by ...
1 - Stars: Introduction
... Huge, very hot, blue star. It is a post-main sequence star that burns helium. ...
... Huge, very hot, blue star. It is a post-main sequence star that burns helium. ...
Which Stars Form Black Holes and Neutron Stars?
... could be a link between massive stars and the presence of strong magnetic fields in their remnants. However, it is not clear when the strong fields of magnetars are generated. One possibility is that they are produced by a dynamo that forms when the core of a rapidly-rotating star collapses [62]. In ...
... could be a link between massive stars and the presence of strong magnetic fields in their remnants. However, it is not clear when the strong fields of magnetars are generated. One possibility is that they are produced by a dynamo that forms when the core of a rapidly-rotating star collapses [62]. In ...
The Galactic Halo
... Stars with enhanced abundances of carbon (CEMP stars), and other light elements (including the lowest [Fe/H] star yet discovered), and lack of over-abundances of neutron-capture elements (CEMP-no stars) Associated with production by “faint SNe” – progenitors with mass on the order of 10-100 Mo under ...
... Stars with enhanced abundances of carbon (CEMP stars), and other light elements (including the lowest [Fe/H] star yet discovered), and lack of over-abundances of neutron-capture elements (CEMP-no stars) Associated with production by “faint SNe” – progenitors with mass on the order of 10-100 Mo under ...
Astronomy 112: The Physics of Stars Class 17 Notes: Core Collapse
... One important effect that distinguishes the evolution of massive stars from that of lower mass stars is the importance of mass loss, both on the main sequence and thereafter. Low mass stars do not experience significant mass loss before the AGB phase, but massive stars, as we have already seen, can ...
... One important effect that distinguishes the evolution of massive stars from that of lower mass stars is the importance of mass loss, both on the main sequence and thereafter. Low mass stars do not experience significant mass loss before the AGB phase, but massive stars, as we have already seen, can ...
Lecture 5: The Milky Way
... The Thin Disk: what fuels ongoing star formation? • The Milky Way is forming stars at ~1-5 solar masses/year, essentially all of it in the thin disk. Where is the gas coming from? • Stripped from satellites? Accreted through filaments? ...
... The Thin Disk: what fuels ongoing star formation? • The Milky Way is forming stars at ~1-5 solar masses/year, essentially all of it in the thin disk. Where is the gas coming from? • Stripped from satellites? Accreted through filaments? ...
Eclipsing binary stars
... or is too close to its brighter companion, we cannot observe both components of the double system with telescope. That this bright star has a companion we detect by astrometric methods. Astrometry measures and explains the positions and movements of stars and other celestial bodies. If only one star ...
... or is too close to its brighter companion, we cannot observe both components of the double system with telescope. That this bright star has a companion we detect by astrometric methods. Astrometry measures and explains the positions and movements of stars and other celestial bodies. If only one star ...
III Ionized Hydrogen (HII) Regions
... “Classical HII Regions” ionized by hot O or B stars (or clusters of such stars) and associated with regions of recent massive-star formation, and “Planetary Nebulae”, the ejected outer envelopes of AGB stars photoionized by the hot remnant stellar core. While the physical origins of these types of g ...
... “Classical HII Regions” ionized by hot O or B stars (or clusters of such stars) and associated with regions of recent massive-star formation, and “Planetary Nebulae”, the ejected outer envelopes of AGB stars photoionized by the hot remnant stellar core. While the physical origins of these types of g ...
幻灯片 1
... clusters with varied age, mass and metallicity The frequency of debris disk and its life time versus the mass, metallicity of the host star C: Detect the spin of stars by analysis their light curves The relation between spin, age and mass of star Higher certainties on the mass, radius of planet ...
... clusters with varied age, mass and metallicity The frequency of debris disk and its life time versus the mass, metallicity of the host star C: Detect the spin of stars by analysis their light curves The relation between spin, age and mass of star Higher certainties on the mass, radius of planet ...
lecture2 - X-Ray
... In 60s the first X-ray sources have been discovered. They were neutron stars in close binary systems, BUT ... .... they were «not recognized».... Now we know hundreds of X-ray binaries with neutron stars in the Milky Way and in other ...
... In 60s the first X-ray sources have been discovered. They were neutron stars in close binary systems, BUT ... .... they were «not recognized».... Now we know hundreds of X-ray binaries with neutron stars in the Milky Way and in other ...
Sin título de diapositiva - Universitat de Barcelona
... The GAIA mission, the next ESA Cornerstone 6 (launch 2010- 2012), will create a precise three dimensional map of about one billion stars throughout our Galaxy and beyond. To reach the scientific goals, that is to quantify the dynamical, chemical and star formation evolution of the Milky Way, it is c ...
... The GAIA mission, the next ESA Cornerstone 6 (launch 2010- 2012), will create a precise three dimensional map of about one billion stars throughout our Galaxy and beyond. To reach the scientific goals, that is to quantify the dynamical, chemical and star formation evolution of the Milky Way, it is c ...
Adaptive Optics at the Keck Observatory: Goals and Near
... the current AO system needs to be understood and fixed. Work is currently underway which could answer these questions. This work needs to be given extremely high priority and support. Near-term opportunities also exist for performing important clearly needed upgrades to the current system. One such ...
... the current AO system needs to be understood and fixed. Work is currently underway which could answer these questions. This work needs to be given extremely high priority and support. Near-term opportunities also exist for performing important clearly needed upgrades to the current system. One such ...
Planetary nebula
A planetary nebula, often abbreviated as PN or plural PNe, is a kind of emission nebula consisting of an expanding glowing shell of ionized gas ejected from old red giant stars late in their lives. The word ""nebula"" is Latin for mist or cloud and the term ""planetary nebula"" is a misnomer that originated in the 1780s with astronomer William Herschel because when viewed through his telescope, these objects appeared to him to resemble the rounded shapes of planets. Herschel's name for these objects was popularly adopted and has not been changed. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion years.A mechanism for formation of most planetary nebulae is thought to be the following: at the end of the star's life, during the red giant phase, the outer layers of the star are expelled by strong stellar winds. Eventually, after most of the red giant's atmosphere is dissipated, the exposed hot, luminous core emits ultraviolet radiation to ionize the ejected outer layers of the star. Absorbed ultraviolet light energises the shell of nebulous gas around the central star, appearing as a bright coloured planetary nebula at several discrete visible wavelengths.Planetary nebulae may play a crucial role in the chemical evolution of the Milky Way, returning material to the interstellar medium from stars where elements, the products of nucleosynthesis (such as carbon, nitrogen, oxygen and neon), have been created. Planetary nebulae are also observed in more distant galaxies, yielding useful information about their chemical abundances.In recent years, Hubble Space Telescope images have revealed many planetary nebulae to have extremely complex and varied morphologies. About one-fifth are roughly spherical, but the majority are not spherically symmetric. The mechanisms which produce such a wide variety of shapes and features are not yet well understood, but binary central stars, stellar winds and magnetic fields may play a role.