Statistical analysis of stellar evolution
... its dominant position in a CMD, the evolved red giants, and the even older white dwarfs. Today the physical processes that govern stellar formation and evolution are studied with complex computer models that can be used to predict the plotted magnitudes on a set of CMDs as a function of stellar para ...
... its dominant position in a CMD, the evolved red giants, and the even older white dwarfs. Today the physical processes that govern stellar formation and evolution are studied with complex computer models that can be used to predict the plotted magnitudes on a set of CMDs as a function of stellar para ...
PPT presentation
... luminosity functions, indistinguishable from those observed in the spiral galaxies M31 and M81. The invariance with galaxy type and metallicity demonstrated the PNLF to be an excellent standard candle. Model simulations indicated a central star mass distribution highly peaked at ~0.6 Msun, similar t ...
... luminosity functions, indistinguishable from those observed in the spiral galaxies M31 and M81. The invariance with galaxy type and metallicity demonstrated the PNLF to be an excellent standard candle. Model simulations indicated a central star mass distribution highly peaked at ~0.6 Msun, similar t ...
Early-type stars in the core of the young open cluster Westerlund 2
... The spectrum of MSP 218 (10:24:07.7, −57:45:41, J2000) is dominated by strong and broad H Balmer lines. Weak absorption lines of He λλ 4388, 4471, Mg λ 4481 and Si λ 4552 are also seen. The He λ 4471/Mg λ 4481 intensity ratio indicates a spectral type B8-A0. The appearance of some we ...
... The spectrum of MSP 218 (10:24:07.7, −57:45:41, J2000) is dominated by strong and broad H Balmer lines. Weak absorption lines of He λλ 4388, 4471, Mg λ 4481 and Si λ 4552 are also seen. The He λ 4471/Mg λ 4481 intensity ratio indicates a spectral type B8-A0. The appearance of some we ...
The HERMES GALAH survey: overview
... and its vertical scale height is about 1000 pc; the scale height of the thin disk is typically about 300 pc. Near the sun, the thick disk is more metal poor, although the abundance ranges of the thick and thin disk stars overlap. The thin disk stars have [Fe/H] in the range 0.7 to +0.5, while most o ...
... and its vertical scale height is about 1000 pc; the scale height of the thin disk is typically about 300 pc. Near the sun, the thick disk is more metal poor, although the abundance ranges of the thick and thin disk stars overlap. The thin disk stars have [Fe/H] in the range 0.7 to +0.5, while most o ...
Surface Gravity as a Diagnostic ... Youth Cameron Higby-Naquin Advisor: Eric Jensen
... fusion in its core and attains full hydrostatic equilibrium. The fact that young stars do not possess these two qualities emphasizes the differences between middle aged stars and stars that are still forming. The study of the evolutionary stages that span a star's youth has been a very active field ...
... fusion in its core and attains full hydrostatic equilibrium. The fact that young stars do not possess these two qualities emphasizes the differences between middle aged stars and stars that are still forming. The study of the evolutionary stages that span a star's youth has been a very active field ...
NSDL/NSTA Web Seminar: Celebrating Astronomy: A Star`s Story
... evolves and eventually dies is its initial mass. ...
... evolves and eventually dies is its initial mass. ...
Searching for the oldest, most metal-poor stars in the SkyMapper Survey
... 1. Normalize the spectra. The processed and reduced echelle spectra from the MagellanClay telescope for each star are high-resolution (0.7” slit R = λ/∆λ ∼ 30, 000 and 1.0” slit R ∼ 35, 000) line spectra. Each spectrum possess ∼ 30 orders, which are small pieces of the spectrum. The wavelength rang ...
... 1. Normalize the spectra. The processed and reduced echelle spectra from the MagellanClay telescope for each star are high-resolution (0.7” slit R = λ/∆λ ∼ 30, 000 and 1.0” slit R ∼ 35, 000) line spectra. Each spectrum possess ∼ 30 orders, which are small pieces of the spectrum. The wavelength rang ...
The Classification of Stellar Spectra
... prominence of certain spectral lines. In Secchi’s scheme, for instance, stars with very strong hydrogen lines were called type I, stars with strong lines from metallic ions like iron and calcium were called type II, stars with wide bands of absorption that got darker toward the blue were called type ...
... prominence of certain spectral lines. In Secchi’s scheme, for instance, stars with very strong hydrogen lines were called type I, stars with strong lines from metallic ions like iron and calcium were called type II, stars with wide bands of absorption that got darker toward the blue were called type ...
Star 1 A star is a massive, luminous ball of plasma held together by
... equilibrium, a protostar forms at the core.[56] These pre–main sequence stars are often surrounded by a protoplanetary disk. The period of gravitational contraction lasts for about 10–15 million years. Early stars of less than 2 solar masses are Artist's conception of the birth of a star within a de ...
... equilibrium, a protostar forms at the core.[56] These pre–main sequence stars are often surrounded by a protoplanetary disk. The period of gravitational contraction lasts for about 10–15 million years. Early stars of less than 2 solar masses are Artist's conception of the birth of a star within a de ...
Lecture18
... Stars form in very large, cold interstellar clouds composed of molecular hydrogen and dust called, molecular clouds. These molecular clouds sit between the stars in the Galaxy. The are very cold (10 K) so we can only see them with infrared and radio telescopes ...
... Stars form in very large, cold interstellar clouds composed of molecular hydrogen and dust called, molecular clouds. These molecular clouds sit between the stars in the Galaxy. The are very cold (10 K) so we can only see them with infrared and radio telescopes ...
Galaxies - science9atsouthcarletonhs
... as “spiral nebulae” and most astronomers believed them to be clouds of gas and stars associated with our own Milky Way. The breakthrough came in 1924 when Edwin Hubble was able to measure the distance to the “Great Nebula in Andromeda” (M 31, at right) and found its distance to be much larger than t ...
... as “spiral nebulae” and most astronomers believed them to be clouds of gas and stars associated with our own Milky Way. The breakthrough came in 1924 when Edwin Hubble was able to measure the distance to the “Great Nebula in Andromeda” (M 31, at right) and found its distance to be much larger than t ...
Discovery of White Dwarfs—1 Oct • Adams’ discovery
... • How much smaller is Sirius B? • Apparent mag of Sirius A is −1.5 • Apparent mag of Sirius B is 8.7 ...
... • How much smaller is Sirius B? • Apparent mag of Sirius A is −1.5 • Apparent mag of Sirius B is 8.7 ...
VY Canis Majoris: The Astrophysical Basis of Its Luminosity
... gives Tef f ∼ 3450–3535◦, while an older scale (used in Humphreys & McElroy 1984 from Flower 1977) yields Tef f ∼ 3200◦ for an M4-M5 star. However, one should be cautious in the case of VY CMa; we are not observing either its photosphere or its surface directly. It has been known for some time that ...
... gives Tef f ∼ 3450–3535◦, while an older scale (used in Humphreys & McElroy 1984 from Flower 1977) yields Tef f ∼ 3200◦ for an M4-M5 star. However, one should be cautious in the case of VY CMa; we are not observing either its photosphere or its surface directly. It has been known for some time that ...
A History of Star Catalogues - The Albuquerque Astronomical Society
... year or 1.4 degrees per century. So when a star’s position is given, the time of observation must also be given. A star catalog may take years or decades to compile, and it is useful to mathematically back out the precession and make all the measurements appear to be made at the same time. The data ...
... year or 1.4 degrees per century. So when a star’s position is given, the time of observation must also be given. A star catalog may take years or decades to compile, and it is useful to mathematically back out the precession and make all the measurements appear to be made at the same time. The data ...
WHAT MAKES A STAR SO SPECIAL Abstract
... 1. The teacher introduces the physical characteristics of stars and the spectral classification to the students (you can use the information from the Introduction section as a supplement to the lesson about Star characteristics in the textbook you are using). 2. The teacher gives every student an en ...
... 1. The teacher introduces the physical characteristics of stars and the spectral classification to the students (you can use the information from the Introduction section as a supplement to the lesson about Star characteristics in the textbook you are using). 2. The teacher gives every student an en ...
Infrared Properties of Star-Forming Dwarf Galaxies. I. Dwarf Irregular
... the NIR light of dIs can be considered to be predominantly contributed by stars older than about 4 Gyr. Although exponential at large radii, surface brightness profiles for the unresolved component flatten in the centers. They can be fitted across the whole range of radii with a hyperbolic secant (s ...
... the NIR light of dIs can be considered to be predominantly contributed by stars older than about 4 Gyr. Although exponential at large radii, surface brightness profiles for the unresolved component flatten in the centers. They can be fitted across the whole range of radii with a hyperbolic secant (s ...
a changing cosmos - Whittier Union High School District
... is found to be on a collision course with Earth, so that an effort could be made to divert it. Currently, NASA carries out the “Spaceguard Survey” to find NEOs greater than 140 meters in diameter, and this program was budgeted at $4.1 million per year for FY 2006 through FY 2012. In chapter 7, we'll ...
... is found to be on a collision course with Earth, so that an effort could be made to divert it. Currently, NASA carries out the “Spaceguard Survey” to find NEOs greater than 140 meters in diameter, and this program was budgeted at $4.1 million per year for FY 2006 through FY 2012. In chapter 7, we'll ...
PDF Full-text
... at these atmospheric levels. This calculation does not include the rest of the observed UV flux from GJ 436 or the flux in the 91.2–120 nm band that is important for the photodissociation of CO and CO2 . For hot Jupiters, Moses et al. [9] compared photochemical to equilibrium models assuming both ox ...
... at these atmospheric levels. This calculation does not include the rest of the observed UV flux from GJ 436 or the flux in the 91.2–120 nm band that is important for the photodissociation of CO and CO2 . For hot Jupiters, Moses et al. [9] compared photochemical to equilibrium models assuming both ox ...
A very massive runaway star from Cygnus OB2⋆
... of motion in the plane of the sky by means of the symmetry axis of the well-dened bow shock, which matches well the orientation ...
... of motion in the plane of the sky by means of the symmetry axis of the well-dened bow shock, which matches well the orientation ...
Long-term monitoring of the short period SU UMa
... the system kept almost constant magnitude until the end of our run. Such a halt is sometimes observed in other SU UMa-type dwarf novae (e.g., V1028 Cyg, Baba et al. 2000. For a comprehensive review, see Kato et al. 2003). On HJD 2452425, 12 days after the detection of the outburst, V844 Her likely e ...
... the system kept almost constant magnitude until the end of our run. Such a halt is sometimes observed in other SU UMa-type dwarf novae (e.g., V1028 Cyg, Baba et al. 2000. For a comprehensive review, see Kato et al. 2003). On HJD 2452425, 12 days after the detection of the outburst, V844 Her likely e ...
Galaxies
... compare the space between the galaxies to their sizes we find that, on the average, they are separated by about 10 to 100 times of their diameter. Hence, there would be a large number of collisions. Large telescopes reveal hundreds of galaxies that appear to be colliding with other galaxies. One of ...
... compare the space between the galaxies to their sizes we find that, on the average, they are separated by about 10 to 100 times of their diameter. Hence, there would be a large number of collisions. Large telescopes reveal hundreds of galaxies that appear to be colliding with other galaxies. One of ...
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.