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The High Resolution Camera CXC Newsletter
... and activity periods). 129 sources could be classified as X-ray binaries due to their position in globular clusters or their strong time variability (see Fig. 2). We detected seven supernova remnants, one of which is a new candidate, and also resolved the first X-rays from a known radio supernova re ...
... and activity periods). 129 sources could be classified as X-ray binaries due to their position in globular clusters or their strong time variability (see Fig. 2). We detected seven supernova remnants, one of which is a new candidate, and also resolved the first X-rays from a known radio supernova re ...
Astrometric accuracy during the past 2000 years
... Internal errors of observations are obtained by analysis of repeated observations of the same stars at different times, as is usually done in meridian observation catalogues, e.g. in case of USNO (1920) from the n=10 observations. I have then derived the error for Table 1 by division with sqrt(10) b ...
... Internal errors of observations are obtained by analysis of repeated observations of the same stars at different times, as is usually done in meridian observation catalogues, e.g. in case of USNO (1920) from the n=10 observations. I have then derived the error for Table 1 by division with sqrt(10) b ...
Ch17_Galaxies
... • The Milky Way belongs to a very small cluster called the Local Group • The Local Group contains about 30 members with the 3 largest members being the spiral galaxies M31, M33, and the Milky Way • Most of the Local Group galaxies are faint, small “dwarf” galaxies - ragged, disorganized collection o ...
... • The Milky Way belongs to a very small cluster called the Local Group • The Local Group contains about 30 members with the 3 largest members being the spiral galaxies M31, M33, and the Milky Way • Most of the Local Group galaxies are faint, small “dwarf” galaxies - ragged, disorganized collection o ...
Luminosities and mass-loss rates of SMC and LMC AGB stars and
... interstellar medium, AGB stars are key players in the life cycle of dust and gas in the universe. However, a quantitative understanding of the mass-loss process is still largely lacking, particularly its dependence on metallicity. Aims. To investigate the relation between mass loss, luminosity and p ...
... interstellar medium, AGB stars are key players in the life cycle of dust and gas in the universe. However, a quantitative understanding of the mass-loss process is still largely lacking, particularly its dependence on metallicity. Aims. To investigate the relation between mass loss, luminosity and p ...
Research Papers-Cosmology/Download/6307
... obviously because the stars in the galaxy's core separated from each other over long distances and do not constitute a single body. The figure of the spiral galaxy also says that the galactic vortex of the dark gas actively generates the velocities of the stars and their positions relative to the ce ...
... obviously because the stars in the galaxy's core separated from each other over long distances and do not constitute a single body. The figure of the spiral galaxy also says that the galactic vortex of the dark gas actively generates the velocities of the stars and their positions relative to the ce ...
Exposing the hidden white dwarf binary origin by means of a
... dwarfs (WDs), including effective temperature and mass distribution. The only two parameters of the synthetic population model are the initial mass function (IMF) and the star-formation rate (SFR). Depletion losses through kinematic heating of the stellar ‘gas’ vertical to the Galactic plane are pre ...
... dwarfs (WDs), including effective temperature and mass distribution. The only two parameters of the synthetic population model are the initial mass function (IMF) and the star-formation rate (SFR). Depletion losses through kinematic heating of the stellar ‘gas’ vertical to the Galactic plane are pre ...
PPT presentation
... • Distance determination using the PN luminosity function (PNLF). • PNs as kinematic probes: dark matter and angular momentum distribution. PN detections at large angular distances from the galaxy’s center are especially valuable; they provide unique information. • Intracluster PNs; tracers of an in ...
... • Distance determination using the PN luminosity function (PNLF). • PNs as kinematic probes: dark matter and angular momentum distribution. PN detections at large angular distances from the galaxy’s center are especially valuable; they provide unique information. • Intracluster PNs; tracers of an in ...
Bluffer`s Guide to Sirius
... successfully bluff your way in astronomy, you will know to pause and calmly announce the answer to be “the Sun”. Apart from the Sun then? Sirius is the brightest star in the night sky. Many nonastronomers believe that the Pole star (Polaris) is the brightest star. If any of your audience suggest thi ...
... successfully bluff your way in astronomy, you will know to pause and calmly announce the answer to be “the Sun”. Apart from the Sun then? Sirius is the brightest star in the night sky. Many nonastronomers believe that the Pole star (Polaris) is the brightest star. If any of your audience suggest thi ...
Stellar populations in the nuclear regions of nearby radio galaxies
... were unable to acquire the red spectrum of the corresponding standard because of a technical failure. One calibration lamp CuAr+CuNe exposure per spectral region and telescope position was also obtained for all objects. The total integration times for the radio galaxies (from 1–3 hrÞ were split into ...
... were unable to acquire the red spectrum of the corresponding standard because of a technical failure. One calibration lamp CuAr+CuNe exposure per spectral region and telescope position was also obtained for all objects. The total integration times for the radio galaxies (from 1–3 hrÞ were split into ...
Harappan Astronomy
... However, the seasons in the Indian Subcontinent are driven by a different set of parameters compared to what happens at higher latitudes (from which we had taken the earlier definition since the Sun never comes overhead in higher latitudes). For the Subcontinent we can define the seasons as follows: ...
... However, the seasons in the Indian Subcontinent are driven by a different set of parameters compared to what happens at higher latitudes (from which we had taken the earlier definition since the Sun never comes overhead in higher latitudes). For the Subcontinent we can define the seasons as follows: ...
Reassessing the formation of the inner Oort cloud
... stellar encounters with the outer Solar System as hyperbolic fly-bys. Second, we have included the expulsion of the cluster gas, a feature that was absent previously. Third, we have used several models for the initial conditions and density profile of the cluster – either a Hernquist or Plummer pote ...
... stellar encounters with the outer Solar System as hyperbolic fly-bys. Second, we have included the expulsion of the cluster gas, a feature that was absent previously. Third, we have used several models for the initial conditions and density profile of the cluster – either a Hernquist or Plummer pote ...
The spectroscopic Hertzsprung
... to the surfaces of the stars (modeled or observed) needs to be the same for all stars considered in the diagram. As mentioned above, this is approximately given for hot stars with the same hydrogen abundance, and thus holds for most Galactic OB stars. For helium-enriched hot stars, their Eddington f ...
... to the surfaces of the stars (modeled or observed) needs to be the same for all stars considered in the diagram. As mentioned above, this is approximately given for hot stars with the same hydrogen abundance, and thus holds for most Galactic OB stars. For helium-enriched hot stars, their Eddington f ...
Can we account for the dust
... M.J. Barlow, G.C. Sloan, A.A. Zijlstra, D. Stock, P.A. Whitelock, P. R. Wood, M.-R.L. Cioni, M.A.T. Groenewegen, K.Volk, J. Bernard-Salas, F. Kemper, T. Kodama, E. Lagadec, M. Meixner, S. Srinivasan, C. Szyszka, J.Th. van Loon ...
... M.J. Barlow, G.C. Sloan, A.A. Zijlstra, D. Stock, P.A. Whitelock, P. R. Wood, M.-R.L. Cioni, M.A.T. Groenewegen, K.Volk, J. Bernard-Salas, F. Kemper, T. Kodama, E. Lagadec, M. Meixner, S. Srinivasan, C. Szyszka, J.Th. van Loon ...
transcript.
... ANDREA GHEZ: Our view to the center of the galaxy is absolutely superb. And our ability to position stars at the center of the galaxy is like somebody in Los Angeles seeing somebody in New York be able to move their fingers, like this, okay? Just two centimeters. That's the precision with which we c ...
... ANDREA GHEZ: Our view to the center of the galaxy is absolutely superb. And our ability to position stars at the center of the galaxy is like somebody in Los Angeles seeing somebody in New York be able to move their fingers, like this, okay? Just two centimeters. That's the precision with which we c ...
A trio of metalrich dust and gas discs found orbiting candidate white
... measurements and optical spectroscopy of six white dwarf candidates selected for apparent K-band excess fluxes based on the ground-based photometric surveys: the Sloan Digital Sky Survey (SDSS) and the UKIRT Infrared Deep Sky Survey (UKIDSS). Target selection criteria and survey data are given in Se ...
... measurements and optical spectroscopy of six white dwarf candidates selected for apparent K-band excess fluxes based on the ground-based photometric surveys: the Sloan Digital Sky Survey (SDSS) and the UKIRT Infrared Deep Sky Survey (UKIDSS). Target selection criteria and survey data are given in Se ...
Effects of triple-α and C(α, γ )16 O reaction rates on the supernova
... Apart from appearances of observations, we can see the effects of the OKK rate on stellar evolution from the ignition properties. A helium core flash is triggered if the nuclear energy generation rates (εn ) become significantly larger than the neutrino energy loss rates (εν ). We can understand cle ...
... Apart from appearances of observations, we can see the effects of the OKK rate on stellar evolution from the ignition properties. A helium core flash is triggered if the nuclear energy generation rates (εn ) become significantly larger than the neutrino energy loss rates (εν ). We can understand cle ...
east and west encounter at sea
... was populated since 1431/2, and the voyage was an ocean trip of more than 800 miles. So, they performed not only coastal voyages, in which case the dead reckoning navigation would be sufficient. It was necessary to know with a certain amount of accuracy the position of the ship on the high seas. In ...
... was populated since 1431/2, and the voyage was an ocean trip of more than 800 miles. So, they performed not only coastal voyages, in which case the dead reckoning navigation would be sufficient. It was necessary to know with a certain amount of accuracy the position of the ship on the high seas. In ...
P7 Further Physics
... Astronomers often use the “parsec” to describe galactic distances. A parsec is roughly 3¼ light years. Angles involved in parallax measurements are often very small and are measured in seconds of an arc (arcseconds). A second of an arc is 1/60th of a minute of an arc, which is 1/60th of a degree. In ...
... Astronomers often use the “parsec” to describe galactic distances. A parsec is roughly 3¼ light years. Angles involved in parallax measurements are often very small and are measured in seconds of an arc (arcseconds). A second of an arc is 1/60th of a minute of an arc, which is 1/60th of a degree. In ...
Table of Contents - Imiloa Astronomy Center
... was, is purported to have asked Job if he (Job) was able to “loose the bands of Orion” (Job ...
... was, is purported to have asked Job if he (Job) was able to “loose the bands of Orion” (Job ...
Test Ch. 27 Multiple Choice Identify the choice that best completes
... 25. In the last stage of stellar evolution following a supernova, stars too massive to form neutron stars may form a A. black dwarf. B. red supergiant. C. white dwarf. D. black hole. 26. In which stage of stellar evolution does combined hydrogen fusion and helium fusion cause a star’s outer shell to ...
... 25. In the last stage of stellar evolution following a supernova, stars too massive to form neutron stars may form a A. black dwarf. B. red supergiant. C. white dwarf. D. black hole. 26. In which stage of stellar evolution does combined hydrogen fusion and helium fusion cause a star’s outer shell to ...
Stellar kinematics
Stellar kinematics is the study of the movement of stars without needing to understand how they acquired their motion. This differs from stellar dynamics, which takes into account gravitational effects. The motion of a star relative to the Sun can provide useful information about the origin and age of a star, as well as the structure and evolution of the surrounding part of the Milky Way.In astronomy, it is widely accepted that most stars are born within molecular clouds known as stellar nurseries. The stars formed within such a cloud compose open clusters containing dozens to thousands of members. These clusters dissociate over time. Stars that separate themselves from the cluster's core are designated as members of the cluster's stellar association. If the remnant later drifts through the Milky Way as a coherent assemblage, then it is termed a moving group.