Wolf-Rayet Stars
... tendency to refer to WN stars of classes 2 to 5 as early type (WNE) and classes 6 to 9 as late type (WNL). Similarly WC4-6 stars are designated as WCE, while WC7-9 stars are designated as WCL. Although there are important exceptions, WNE stars generally show no evidence for H emission while H emissi ...
... tendency to refer to WN stars of classes 2 to 5 as early type (WNE) and classes 6 to 9 as late type (WNL). Similarly WC4-6 stars are designated as WCE, while WC7-9 stars are designated as WCL. Although there are important exceptions, WNE stars generally show no evidence for H emission while H emissi ...
Sample pages 1 PDF
... more precise measurements of declination the degree is divided into 60 arcmin (0 ), and an arc minute is divided into 60 arcsec (00 ) (Figure 2.8). The selection of the coordinate starting point for the right ascension is – the same as on Earth – a matter of choice. In the same way as all geographic ...
... more precise measurements of declination the degree is divided into 60 arcmin (0 ), and an arc minute is divided into 60 arcsec (00 ) (Figure 2.8). The selection of the coordinate starting point for the right ascension is – the same as on Earth – a matter of choice. In the same way as all geographic ...
Processing of Star Catalog and Star Image
... areas in order to guarantee that the distribution of guide stars in the entire celestial area is as even as possible. Based on the single magnitude threshold, there are too many stars in the FOV as a result of some boresight pointings, while there are no stars in the FOV of some celestial areas. Obv ...
... areas in order to guarantee that the distribution of guide stars in the entire celestial area is as even as possible. Based on the single magnitude threshold, there are too many stars in the FOV as a result of some boresight pointings, while there are no stars in the FOV of some celestial areas. Obv ...
Luminosity, Flux and Magnitudes Outline
... h = Planck’s constant, k = Boltzmann’s constant, c = speed of light This is the power radiated per unit area in the frequency range to + d into a unit solid angle (d = d sin d in spherical ...
... h = Planck’s constant, k = Boltzmann’s constant, c = speed of light This is the power radiated per unit area in the frequency range to + d into a unit solid angle (d = d sin d in spherical ...
Notes on Stars
... Bolometric magnitudes mbol are a measure for the total luminosity integrated over all wavelengths. One defines: ...
... Bolometric magnitudes mbol are a measure for the total luminosity integrated over all wavelengths. One defines: ...
Abstract book
... Title: Asymptotic Giant Branch stars in intermediate age clusters Abstract. Spectroscopic and photometric observations of AGB stars belonging to intermediate age clusters (1 to 3 Gyrs) represent one of the most challenging test for the theory of AGB evolution and nucleosynthesis. Their masses (1.3 t ...
... Title: Asymptotic Giant Branch stars in intermediate age clusters Abstract. Spectroscopic and photometric observations of AGB stars belonging to intermediate age clusters (1 to 3 Gyrs) represent one of the most challenging test for the theory of AGB evolution and nucleosynthesis. Their masses (1.3 t ...
Star Formation in the Rosette Complex
... The Rosette Complex (l = 207.0, b = −2.1) is located near the anti-center of the Galactic Disk in the constellation of Monoceros. The region is very popular, partly because of the staggering beauty of its main feature: a very extended emission nebula which hosts a large central HII region, evacuated ...
... The Rosette Complex (l = 207.0, b = −2.1) is located near the anti-center of the Galactic Disk in the constellation of Monoceros. The region is very popular, partly because of the staggering beauty of its main feature: a very extended emission nebula which hosts a large central HII region, evacuated ...
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 ...
Astronomy Astrophysics Circumstellar emission in Be/X-ray binaries of the Magellanic
... Aims. We study the optical and near-infrared colour excesses produced by circumstellar emission in a sample of Be/X-ray binaries. Our main goals are exploring whether previously published relations, valid for isolated Be stars, are applicable to Be/X-ray binaries and computing the distance to these ...
... Aims. We study the optical and near-infrared colour excesses produced by circumstellar emission in a sample of Be/X-ray binaries. Our main goals are exploring whether previously published relations, valid for isolated Be stars, are applicable to Be/X-ray binaries and computing the distance to these ...
a wide-field survey for variable stars
... Tauri variable stars. The nearby dusty, yellow cloud is Hind’s Variable Nebula (NGC 1555/1554). Over 400 light-years away, at the edge of a molecular cloud, both star and nebula are seen to vary significantly in brightness but not necessarily at the same time, adding to the mystery of the intriguing ...
... Tauri variable stars. The nearby dusty, yellow cloud is Hind’s Variable Nebula (NGC 1555/1554). Over 400 light-years away, at the edge of a molecular cloud, both star and nebula are seen to vary significantly in brightness but not necessarily at the same time, adding to the mystery of the intriguing ...
Rotation Periods of Wide Binaries in the Kepler Field
... these clusters are relatively distant, so cluster stars later than early K spectral type are too faint for Kepler. Angus, et al. (2015) used rotation periods of Kepler stars as well as cluster stars and other stars with known ages to derive a period-age-color relation of the form P = aAn (B − V − c) ...
... these clusters are relatively distant, so cluster stars later than early K spectral type are too faint for Kepler. Angus, et al. (2015) used rotation periods of Kepler stars as well as cluster stars and other stars with known ages to derive a period-age-color relation of the form P = aAn (B − V − c) ...
The Nature of the Stars
... against the background of more distant stars (Figure 17-2). This motion is called stellar parallax. The parallax (p) of a star is equal to half the angle through which the star’s apparent position shifts as the Earth moves from one side of its orbit to the other. The larger the parallax p, the small ...
... against the background of more distant stars (Figure 17-2). This motion is called stellar parallax. The parallax (p) of a star is equal to half the angle through which the star’s apparent position shifts as the Earth moves from one side of its orbit to the other. The larger the parallax p, the small ...
Chapter 17--Star Stuff
... The length of time from the formation of a protostar to the birth of a main-sequence star depends on the star’s mass. Massive stars do everything faster. The contraction of a high-mass protostar into a main-sequence star may take only a million years or less. A star like our Sun takes about 50 milli ...
... The length of time from the formation of a protostar to the birth of a main-sequence star depends on the star’s mass. Massive stars do everything faster. The contraction of a high-mass protostar into a main-sequence star may take only a million years or less. A star like our Sun takes about 50 milli ...
Red supergiants around the obscured open cluster Stephenson 2
... (cf. Messineo et al. 2012), this cut selects most RSGs, while leaving out low-luminosity red stars. The vast majority of our targets present a good quality flag (Qflg = A, B, C, or D) in all three 2MASS bands. A few objects with other quality flags were included in the sample and assigned low priori ...
... (cf. Messineo et al. 2012), this cut selects most RSGs, while leaving out low-luminosity red stars. The vast majority of our targets present a good quality flag (Qflg = A, B, C, or D) in all three 2MASS bands. A few objects with other quality flags were included in the sample and assigned low priori ...
The Sky This Month
... • The middle “star” / “fuzzy thing” in Orion’s sword : Mag 4.0. • Bright diffuse nebula with brightest central region about 1° across. • 100 ly away and ~60 ly across. • The closest known star forming region – filled with lots of young stars (Trapezium cluster). • Galileo discovered the Trapezium cl ...
... • The middle “star” / “fuzzy thing” in Orion’s sword : Mag 4.0. • Bright diffuse nebula with brightest central region about 1° across. • 100 ly away and ~60 ly across. • The closest known star forming region – filled with lots of young stars (Trapezium cluster). • Galileo discovered the Trapezium cl ...
12-1 - Piscataway High School
... To make that calculation, you compare the star with the sun. If the corrected absolute magnitude of the star is 1 magnitude brighter than the sun, then it must be 2.5 times more luminous. If it is 5 magnitudes brighter, then it must be 100 times more luminous. Astronomers would write the luminosity ...
... To make that calculation, you compare the star with the sun. If the corrected absolute magnitude of the star is 1 magnitude brighter than the sun, then it must be 2.5 times more luminous. If it is 5 magnitudes brighter, then it must be 100 times more luminous. Astronomers would write the luminosity ...
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.