The Korean 1592--1593 Record of a Guest Star: Animpostor`of the
... that the guest star must be a fixed star because it had been visible for more than three years. This implies that they made self-inspection of their reports on guest stars. The second one is the guest star between the first and second eastern stars of Wangyang, which appeared from November 30, 1592 ...
... that the guest star must be a fixed star because it had been visible for more than three years. This implies that they made self-inspection of their reports on guest stars. The second one is the guest star between the first and second eastern stars of Wangyang, which appeared from November 30, 1592 ...
On the nature and detectability of Type Ib/c supernova progenitors
... To compute BC = Mbol − MV , we adopt Mv − MV = 0.75 to correct for the effect of strong emission lines on the visual broadband magnitude MV (cf. Crockett et al. 2007). The BCs calculated by Maund et al. (2005) using the Potsdam WR grid are plotted in the same figure for comparison. Here again, the f ...
... To compute BC = Mbol − MV , we adopt Mv − MV = 0.75 to correct for the effect of strong emission lines on the visual broadband magnitude MV (cf. Crockett et al. 2007). The BCs calculated by Maund et al. (2005) using the Potsdam WR grid are plotted in the same figure for comparison. Here again, the f ...
Riccioli Measures the Stars: Observations of the
... diameter of (fixed) stars depends upon observing planets and comparing planetary and stellar diameters; he refers the reader to Book 6 Chapter IX for discussion of the diameters of stars and planets and their measurement. He and Grimaldi record the shape of Jupiter‟s disk and Saturn‟s oval form, emp ...
... diameter of (fixed) stars depends upon observing planets and comparing planetary and stellar diameters; he refers the reader to Book 6 Chapter IX for discussion of the diameters of stars and planets and their measurement. He and Grimaldi record the shape of Jupiter‟s disk and Saturn‟s oval form, emp ...
Cataclysmic Cosmic Events and How to Observe Them www.springer.com/series/5338
... GRBs currently battle for the record of the most distant, highest redshift objects known; the former shine at us across billions of light-years due to the radiation from the nucleus of a galaxy surrounding a billion-solar-mass black hole. The latter, in the most violent cases, shine briefly but viol ...
... GRBs currently battle for the record of the most distant, highest redshift objects known; the former shine at us across billions of light-years due to the radiation from the nucleus of a galaxy surrounding a billion-solar-mass black hole. The latter, in the most violent cases, shine briefly but viol ...
Age-Dating of Young Stars and Stellar Systems
... is very different from, e.g., a globular cluster isochrone where most of the luminosity comes from a small mass interval close to the turn-off mass. In a typical massive-star population of single age, stars with vastly different zero-age-mainsequence masses can have similar Teff and L and contribute ...
... is very different from, e.g., a globular cluster isochrone where most of the luminosity comes from a small mass interval close to the turn-off mass. In a typical massive-star population of single age, stars with vastly different zero-age-mainsequence masses can have similar Teff and L and contribute ...
The first photometric analysis of the overcontact binary MQ UMa with
... The equation is derived from a total sample of 141 contact binaries, whose spectral type ranges from A2V to K5V, and has a period from 0.2211 days to 1.1318 days. The sample has covered nearly all kinds of W UMa type contact binaries which means it is appropriate to MQ UMa. The period of MQ UMa is 0 ...
... The equation is derived from a total sample of 141 contact binaries, whose spectral type ranges from A2V to K5V, and has a period from 0.2211 days to 1.1318 days. The sample has covered nearly all kinds of W UMa type contact binaries which means it is appropriate to MQ UMa. The period of MQ UMa is 0 ...
Neon abundances - UCL Astrophysics Group
... In many cases, the lines are so weak that only upper limits can be established. The most extreme example found is y Her with an underabundance of at least 1.5 dex. These underabundances are qualitatively expected from radiative acceleration calculations, which show that Ne has a very small radiative ...
... In many cases, the lines are so weak that only upper limits can be established. The most extreme example found is y Her with an underabundance of at least 1.5 dex. These underabundances are qualitatively expected from radiative acceleration calculations, which show that Ne has a very small radiative ...
Chapter 1 The Discovery of Open Clusters - Willmann-Bell
... Very compressed, rich clusters of stars Compressed clusters of small and large stars Coarsely scattered clusters of stars. Although now long superseded, the Herschel designations which resulted from this classification system proved sufficiently useful that they were often used by amateur astronomer ...
... Very compressed, rich clusters of stars Compressed clusters of small and large stars Coarsely scattered clusters of stars. Although now long superseded, the Herschel designations which resulted from this classification system proved sufficiently useful that they were often used by amateur astronomer ...
Star Formation in the Rosette Complex
... map of the Rosette Complex using the Arecibo telescope. They found that neutral gas in the Rosette Complex is distributed in three main regions which form a rough, extended shell of about 45 pc in radius around the nebula and extend beyond the molecular cloud. This shell would have a center of expan ...
... map of the Rosette Complex using the Arecibo telescope. They found that neutral gas in the Rosette Complex is distributed in three main regions which form a rough, extended shell of about 45 pc in radius around the nebula and extend beyond the molecular cloud. This shell would have a center of expan ...
Milky Way Galaxy
... The Universe is filled with these star systems which themselves cluster together into larger systems. ...
... The Universe is filled with these star systems which themselves cluster together into larger systems. ...
doc - Pocket Stars
... an improved fix from two or more LOPs. You can select from amongst the previously acquired observations by checking the associated checkbox. The results are shown in red text in the lower left corner. These include: ...
... an improved fix from two or more LOPs. You can select from amongst the previously acquired observations by checking the associated checkbox. The results are shown in red text in the lower left corner. These include: ...
White dwarfs from GAIA: The 7th dimension
... • The white dwarf luminosity function of Gaia is a sensitive probe of the averaged star formation rate • Due to their very short main-sequence lifetimes the shape of the SFR can be reconstructed from the luminosity function of massive white dwarfs • To achieve these goals, we need R~5000 spectroscop ...
... • The white dwarf luminosity function of Gaia is a sensitive probe of the averaged star formation rate • Due to their very short main-sequence lifetimes the shape of the SFR can be reconstructed from the luminosity function of massive white dwarfs • To achieve these goals, we need R~5000 spectroscop ...
2 The Concept of “Spectral Classes”
... peculiarities that can appear “globally” across large regions of the HR Diagram. They are mutually duplicative in order to represent as many as two global peculiarities. Codes P3 and P4 are included to specify more fully the peculiarities that often cannot be represented by P1 and P2 alone. Peculiar ...
... peculiarities that can appear “globally” across large regions of the HR Diagram. They are mutually duplicative in order to represent as many as two global peculiarities. Codes P3 and P4 are included to specify more fully the peculiarities that often cannot be represented by P1 and P2 alone. Peculiar ...
November, 2015 - The Baton Rouge Astronomical Society
... small nucleus; two major arms that can be partially resolved with large instruments. M 74 is located ½ ° north and 1 ½ ° east of Eta Piscium. Due to its large size and low surface brightness, M 74 is an elusive object to see. Two supernovae have been observed in M 74, SN 2002ap, and SN 2003gd. Sn200 ...
... small nucleus; two major arms that can be partially resolved with large instruments. M 74 is located ½ ° north and 1 ½ ° east of Eta Piscium. Due to its large size and low surface brightness, M 74 is an elusive object to see. Two supernovae have been observed in M 74, SN 2002ap, and SN 2003gd. Sn200 ...
Distance determination for RAVE stars using stellar models
... spirals, and finally dwarf galaxies. The power spectrum is used to measure the power of density perturbations on a certain scale. The current cosmological model predicts a HarrisonZel’dovich spectrum (P (k) ∝ k, where k is the wavenumber). This power spectrum predicts more power on small scale, so t ...
... spirals, and finally dwarf galaxies. The power spectrum is used to measure the power of density perturbations on a certain scale. The current cosmological model predicts a HarrisonZel’dovich spectrum (P (k) ∝ k, where k is the wavenumber). This power spectrum predicts more power on small scale, so t ...
Activity III: Calibrating Images
... In addition, each CCD reacts differently to light and yields a different number of Counts for a given brightness. In order to use your data in the context of other observations and reference tables, you need to get the brightness of the star in units that are independent of a particular CCD. Calibra ...
... In addition, each CCD reacts differently to light and yields a different number of Counts for a given brightness. In order to use your data in the context of other observations and reference tables, you need to get the brightness of the star in units that are independent of a particular CCD. Calibra ...
to - NexStar Resource Site
... Nebula in the night sky it is almost certainly the easiest Nebula to observe with any size optical instrument. It can also be spotted with the naked eye as a small fuzzy patch below Orions Belt. The Orion Nebula is about 1500 light years distant, located in the same spiral arm of our Galaxy as the S ...
... Nebula in the night sky it is almost certainly the easiest Nebula to observe with any size optical instrument. It can also be spotted with the naked eye as a small fuzzy patch below Orions Belt. The Orion Nebula is about 1500 light years distant, located in the same spiral arm of our Galaxy as the S ...
Trapezium Fracture
... begin to understand the ultimate of their own world? Perhaps these beings will not have evolved on the Orion home worlds at all, but travelled to them from another distant place, and when they peer curiously at our own long dead region of space, it will not be in order to understand their ultimate f ...
... begin to understand the ultimate of their own world? Perhaps these beings will not have evolved on the Orion home worlds at all, but travelled to them from another distant place, and when they peer curiously at our own long dead region of space, it will not be in order to understand their ultimate f ...
Astronomical Picture of the Day
... figure out the cause of unusual jumbles of stars, gas, and dust like NGC 1316. A preliminary inspection indicates that NGC 1316 is an enormous elliptical galaxy that includes dark dust lanes usually found in a spiral. The above image taken by the Hubble Space Telescope shows details, however, that h ...
... figure out the cause of unusual jumbles of stars, gas, and dust like NGC 1316. A preliminary inspection indicates that NGC 1316 is an enormous elliptical galaxy that includes dark dust lanes usually found in a spiral. The above image taken by the Hubble Space Telescope shows details, however, that h ...
Corona Australis
Corona Australis /kɵˈroʊnə ɒˈstreɪlɨs/ or Corona Austrina /kɵˈroʊnə ɒˈstraɪnə/ is a constellation in the Southern Celestial Hemisphere. Its Latin name means ""southern crown"", and it is the southern counterpart of Corona Borealis, the northern crown. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations. The Ancient Greeks saw Corona Australis as a wreath rather than a crown and associated it with Sagittarius or Centaurus. Other cultures have likened the pattern to a turtle, ostrich nest, a tent, or even a hut belonging to a rock hyrax.Although fainter than its namesake, the oval- or horseshoe-shaped pattern of its brighter stars renders it distinctive. Alpha and Beta Coronae Australis are the two brightest stars with an apparent magnitude of around 4.1. Epsilon Coronae Australis is the brightest example of a W Ursae Majoris variable in the southern sky. Lying alongside the Milky Way, Corona Australis contains one of the closest star-forming regions to our Solar System—a dusty dark nebula known as the Corona Australis Molecular Cloud, lying about 430 light years away. Within it are stars at the earliest stages of their lifespan. The variable stars R and TY Coronae Australis light up parts of the nebula, which varies in brightness accordingly.