Searching for the oldest, most metal-poor stars in the SkyMapper Survey
... −2.5 as an initial guess. After every iteration, the metallicity is adjusted based on the estimated abundances from the last iteration. The [α/Fe] ratio is the abundance of α-elements (e.g. magnesium, calcium, and titanium,) divided by the abundance of iron in the star. This parameter was not change ...
... −2.5 as an initial guess. After every iteration, the metallicity is adjusted based on the estimated abundances from the last iteration. The [α/Fe] ratio is the abundance of α-elements (e.g. magnesium, calcium, and titanium,) divided by the abundance of iron in the star. This parameter was not change ...
WORD - Astrophysics
... “dark matter”. The only component that directly retains observable information about star formation rates and metal enrichment rates - the evolution of the baryonic component - is the stellar population. This is because low mass stars have extremely long life times, comparable to the age of the Univ ...
... “dark matter”. The only component that directly retains observable information about star formation rates and metal enrichment rates - the evolution of the baryonic component - is the stellar population. This is because low mass stars have extremely long life times, comparable to the age of the Univ ...
identifying seasonal stars in kaurna astronomical traditions
... Table 2). Many single stars used for calendrical purposes in Aboriginal astronomical traditions are first magnitude (Clarke, 2007; Hamacher ...
... Table 2). Many single stars used for calendrical purposes in Aboriginal astronomical traditions are first magnitude (Clarke, 2007; Hamacher ...
17_Testbank
... A) The giant must once have been the more massive star but transferred some of its mass to its companion. B) Despite the low odds of finding a system with two such massive stars, there is nothing surprising about the fact that such systems exist. C) The two stars probably were once separate but beca ...
... A) The giant must once have been the more massive star but transferred some of its mass to its companion. B) Despite the low odds of finding a system with two such massive stars, there is nothing surprising about the fact that such systems exist. C) The two stars probably were once separate but beca ...
Riccioli Measures the Stars: Observations of the
... have been compelled to choose between an incomprehensibly great magnitude, and a similar motion. Delambre, who comments with brief contempt upon the several arguments of Tycho Brahé, has here only to say, „We should now answer that no star has an apparent diameter of a second.‟ Undoubtedly, but what ...
... have been compelled to choose between an incomprehensibly great magnitude, and a similar motion. Delambre, who comments with brief contempt upon the several arguments of Tycho Brahé, has here only to say, „We should now answer that no star has an apparent diameter of a second.‟ Undoubtedly, but what ...
A very massive runaway star from Cygnus OB2⋆
... Although the identication of BD+43 3654 as a likely runaway star dates back to van Buren & McCray (1988), no spectral classication is available in that work. Subsequent papers by van Buren et al. (1995) and Noriega-Crespo et al. (1997) refer to the star as a unspecied B-type but do not report ded ...
... Although the identication of BD+43 3654 as a likely runaway star dates back to van Buren & McCray (1988), no spectral classication is available in that work. Subsequent papers by van Buren et al. (1995) and Noriega-Crespo et al. (1997) refer to the star as a unspecied B-type but do not report ded ...
Precision age indicators that exploit chemically peculiar stars
... One additional caution about C stars is that they are rare, evolved stars susceptible to stochastic counting effects that can have effects on integrated properties in some cases (Santos & Frogel 1997) though entire, large galaxies are probably immune from stochastic effects. The other, bluer CP stars d ...
... One additional caution about C stars is that they are rare, evolved stars susceptible to stochastic counting effects that can have effects on integrated properties in some cases (Santos & Frogel 1997) though entire, large galaxies are probably immune from stochastic effects. The other, bluer CP stars d ...
1 - Piscataway High School
... represents the star in the H–R diagram moves to the right relatively quickly (in less than a million years for a star of 5 solar masses). A massive star moves to the right across the top of the H–R diagram and becomes a supergiant, while a medium-mass ...
... represents the star in the H–R diagram moves to the right relatively quickly (in less than a million years for a star of 5 solar masses). A massive star moves to the right across the top of the H–R diagram and becomes a supergiant, while a medium-mass ...
Star Formation in the Galaxy, An Observational Overview
... is again balanced by internal pressure. After this phase such stars will eject their outer atmospheres producing planetary nebula and leaving behind a white dwarf stellar remnant. More massive stars experience a more complex post-main sequence evolution during which they will fuse heavier elements i ...
... is again balanced by internal pressure. After this phase such stars will eject their outer atmospheres producing planetary nebula and leaving behind a white dwarf stellar remnant. More massive stars experience a more complex post-main sequence evolution during which they will fuse heavier elements i ...
Lecture18
... Some stars hot but faint, or cool but very bright: Stars not on the main sequence: giants and super-giants, white dwarfs (all late phases in a star’s lifetime). “Luminosity class” used to distinguish a red main sequence (e.g. M5V) from a red supergiant (M5I). Sizes of stars vary tremendously: White ...
... Some stars hot but faint, or cool but very bright: Stars not on the main sequence: giants and super-giants, white dwarfs (all late phases in a star’s lifetime). “Luminosity class” used to distinguish a red main sequence (e.g. M5V) from a red supergiant (M5I). Sizes of stars vary tremendously: White ...
Mergers of massive main sequence binaries
... with the assumption of no mass loss and homogeneous mixing during the merging process. We find that there are two types of mergers which result from different phases of mass transfer. Both of these types have relatively low hydrogen content which leads to high luminosities. We then used the data of ...
... with the assumption of no mass loss and homogeneous mixing during the merging process. We find that there are two types of mergers which result from different phases of mass transfer. Both of these types have relatively low hydrogen content which leads to high luminosities. We then used the data of ...
Chromospherically young, kinematically old stars
... The chromospheric activity of a late-type star is frequently interpreted as a sign of its youth. Young dwarfs show high rotation rates, and the interaction between rotation and outer envelope convection is expected to drive the chromospheric activity. Nevertheless, not only young single stars presen ...
... The chromospheric activity of a late-type star is frequently interpreted as a sign of its youth. Young dwarfs show high rotation rates, and the interaction between rotation and outer envelope convection is expected to drive the chromospheric activity. Nevertheless, not only young single stars presen ...
Star Clusters - Caltech Astronomy
... stars in the central cluster or clusters and the surrounding association all formed more or less at the same time out of the same material. Since the association is not a gravitationally bound system, after a relatively short period of time, its stars will disperse and the association will lose its ...
... stars in the central cluster or clusters and the surrounding association all formed more or less at the same time out of the same material. Since the association is not a gravitationally bound system, after a relatively short period of time, its stars will disperse and the association will lose its ...
Downloadable Full Text
... The UFD Reticulum II (Ret II) was recently discovered with Dark Energy Survey data12,13 and confirmed to be one of the most metal-poor galaxies known14. On 1-4 Oct 2015, we obtained high-resolution spectra of the nine brightest member stars in Ret II (see Table 1, Extended Data Figure 1). The abunda ...
... The UFD Reticulum II (Ret II) was recently discovered with Dark Energy Survey data12,13 and confirmed to be one of the most metal-poor galaxies known14. On 1-4 Oct 2015, we obtained high-resolution spectra of the nine brightest member stars in Ret II (see Table 1, Extended Data Figure 1). The abunda ...
Star 1 A star is a massive, luminous ball of plasma held together by
... hundreds of thousands of stars located one billion light years away[37] —ten times the distance of the most distant star cluster previously observed. ...
... hundreds of thousands of stars located one billion light years away[37] —ten times the distance of the most distant star cluster previously observed. ...
arXiv:astro-ph/0508448v1 22 Aug 2005
... the SN of its companion must be, or become, massive enough to undergo a WR phase. In the case that mass transfer occurs, the mass limit for a star to go through a WR phase is lowered somewhat (Dray & Tout 2005) due to accretion of He-enhanced matter and subsequent thermohaline mixing. Mass transfer ...
... the SN of its companion must be, or become, massive enough to undergo a WR phase. In the case that mass transfer occurs, the mass limit for a star to go through a WR phase is lowered somewhat (Dray & Tout 2005) due to accretion of He-enhanced matter and subsequent thermohaline mixing. Mass transfer ...
Spectral classification of O–M stars on the basis of UBV photometry
... analyzed stars have been assigned to a single or two rather close estimates of spectra. In the last case an average value was adopted. Another 40% of stars have obtained two substantially different estimates of spectra. Double results of the classifying process based on U BV data originates as a rul ...
... analyzed stars have been assigned to a single or two rather close estimates of spectra. In the last case an average value was adopted. Another 40% of stars have obtained two substantially different estimates of spectra. Double results of the classifying process based on U BV data originates as a rul ...
Table of Contents - Shawnee State University
... Legends of the Night Sky: Orion Educator’s Guide The constellation Draco, the dragon: - Winds between the Big and Little Dippers. - Generally takes up all of the remaining bright stars between those two constellations. - Draco’s head hangs down near Cepheus. - Draco is probably the toughest circump ...
... Legends of the Night Sky: Orion Educator’s Guide The constellation Draco, the dragon: - Winds between the Big and Little Dippers. - Generally takes up all of the remaining bright stars between those two constellations. - Draco’s head hangs down near Cepheus. - Draco is probably the toughest circump ...
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: ...
Building` a Galaxy SED
... Galaxy SED contains information on its stellar populations + star formation history. ...
... Galaxy SED contains information on its stellar populations + star formation history. ...
Auriga (constellation)
Auriga is one of the 48 constellations listed by the 2nd-century astronomer Ptolemy and remains one of the 88 modern constellations. Located north of the celestial equator, its name is the Latin word for ""charioteer"", associating it with various mythological charioteers, including Erichthonius and Myrtilus. Auriga is most prominent during winter evenings in the Northern Hemisphere, along with the five other constellations that have stars in the Winter Hexagon asterism. Because of its northern declination, Auriga is only visible in its entirety as far as 34° south; for observers farther south it lies partially or fully below the horizon. A large constellation, with an area of 657 square degrees, it is half the size of the largest constellation, Hydra.Its brightest star, Capella, is an unusual multiple star system among the brightest stars in the night sky. Beta Aurigae is an interesting variable star in the constellation; Epsilon Aurigae, a nearby eclipsing binary with an unusually long period, has been studied intensively. Because of its position near the winter Milky Way, Auriga has many bright open clusters in its borders, including M36, M37, and M38, popular targets for amateur astronomers. In addition, it has one prominent nebula, the Flaming Star Nebula, associated with the variable star AE Aurigae.In Chinese mythology, Auriga's stars were incorporated into several constellations, including the celestial emperors' chariots, made up of the modern constellation's brightest stars. Auriga is home to the radiant for the Aurigids, Zeta Aurigids, Delta Aurigids, and the hypothesized Iota Aurigids.