DUSTiNGS III: Distribution of Intermediate
... et al. 2007; Vijh et al. 2009), thereby eliminating confusion with other infrared-bright point sources. In total, DUSTiNGS identified 710 variable AGB star candidates including 526 variable x-AGB star candidates (Boyer et al. 2015c, hereafter Paper II). Twelve of these x-AGB star candidates are in g ...
... et al. 2007; Vijh et al. 2009), thereby eliminating confusion with other infrared-bright point sources. In total, DUSTiNGS identified 710 variable AGB star candidates including 526 variable x-AGB star candidates (Boyer et al. 2015c, hereafter Paper II). Twelve of these x-AGB star candidates are in g ...
Galaxy Evolution
... forming stars at a rate of 10 M per year, the galaxy of our example has put together a total stellar mass equal to 10 × 1000 000 = 107 M , about one ten-thousandth of its initial stellar mass. Of these, about 20 000 are massive stars. Because each of these massive stars is 1000 000 times brighter ...
... forming stars at a rate of 10 M per year, the galaxy of our example has put together a total stellar mass equal to 10 × 1000 000 = 107 M , about one ten-thousandth of its initial stellar mass. Of these, about 20 000 are massive stars. Because each of these massive stars is 1000 000 times brighter ...
The low-mass dispersed population around the Lupus clouds
... excesses in the distributed population. Some non-giant members are also identified with gravity-sensitive features typical of more evolved stars, and we argue that these may belong to an older population associated with the Gould Belt, similar to that observed in the direction of other nearby star f ...
... excesses in the distributed population. Some non-giant members are also identified with gravity-sensitive features typical of more evolved stars, and we argue that these may belong to an older population associated with the Gould Belt, similar to that observed in the direction of other nearby star f ...
Galaxy Evolution Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mauro Giavalisco
... forming stars at a rate of 10 M per year, the galaxy of our example has put together a total stellar mass equal to 10 × 1000 000 = 107 M , about one ten-thousandth of its initial stellar mass. Of these, about 20 000 are massive stars. Because each of these massive stars is 1000 000 times brighter ...
... forming stars at a rate of 10 M per year, the galaxy of our example has put together a total stellar mass equal to 10 × 1000 000 = 107 M , about one ten-thousandth of its initial stellar mass. Of these, about 20 000 are massive stars. Because each of these massive stars is 1000 000 times brighter ...
the Local Group - Simon P Driver
... (L > 108 Lsolar), so does not qualify as a cluster – NB, dwarf spheroidals etc. are not detectable at large distances, so don’t make up part of the total galaxy count for the Local Group • about half of known galaxies are in groups and clusters – these are dense enough to halt cosmological expans ...
... (L > 108 Lsolar), so does not qualify as a cluster – NB, dwarf spheroidals etc. are not detectable at large distances, so don’t make up part of the total galaxy count for the Local Group • about half of known galaxies are in groups and clusters – these are dense enough to halt cosmological expans ...
X-Ray Properties of Young Stars and Stellar Clusters
... blue optical/UV continuum, and, in the Sun, high γ-ray and energetic particle fluences. These particles impact the stellar surface at the magnetic footprints, immediately heating gas that flows upward to fill coronal loops with X-ray emitting plasma. It is this “gradual phase” of the flare that is s ...
... blue optical/UV continuum, and, in the Sun, high γ-ray and energetic particle fluences. These particles impact the stellar surface at the magnetic footprints, immediately heating gas that flows upward to fill coronal loops with X-ray emitting plasma. It is this “gradual phase” of the flare that is s ...
THE HELIACAL RISE OF SIRIUS- Algorithm
... The atmospheric extinction for a given place shows how many star-magnitudes are extinguished by one earth atmosphere. In the best case, in a dry mountain desert, the extinction will be around 0.10. In the worse case, around some sea coasts, it may reach 0.40 and even 0.50. There are some scholars wh ...
... The atmospheric extinction for a given place shows how many star-magnitudes are extinguished by one earth atmosphere. In the best case, in a dry mountain desert, the extinction will be around 0.10. In the worse case, around some sea coasts, it may reach 0.40 and even 0.50. There are some scholars wh ...
On the elemental abundance and isotopic mixture of mercury in
... Spectra taken with the EMMI spectrograph at the 3.5 m NTT telescope cover a large wavelength interval (4070– 6740 Å) at a resolving power of R ∼ 80 000 and S/N ∼ 100. The spectrum of AV Scl was taken with the UVES spectrograph at the 8.0 m VLT. The UVES is a two-arm crossdispersed echelle spectrogra ...
... Spectra taken with the EMMI spectrograph at the 3.5 m NTT telescope cover a large wavelength interval (4070– 6740 Å) at a resolving power of R ∼ 80 000 and S/N ∼ 100. The spectrum of AV Scl was taken with the UVES spectrograph at the 8.0 m VLT. The UVES is a two-arm crossdispersed echelle spectrogra ...
sections 23-25 powerpoint
... Elliptical galaxy (E). A spheroidal galaxy containing millions to billions of old low-mass stars and no gas or dust. Spiral Galaxy (S). A galaxy with a spheroidal bulge of several million old low-mass stars and a flattened pancake-like disk of billions of old low-mass and young high-mass stars, alon ...
... Elliptical galaxy (E). A spheroidal galaxy containing millions to billions of old low-mass stars and no gas or dust. Spiral Galaxy (S). A galaxy with a spheroidal bulge of several million old low-mass stars and a flattened pancake-like disk of billions of old low-mass and young high-mass stars, alon ...
3-1
... B. 0.6 + 0.008 + 0.0007 Standard form: 0.6087 Word form: six thousand eighty-seven tenthousandths Course 1 ...
... B. 0.6 + 0.008 + 0.0007 Standard form: 0.6087 Word form: six thousand eighty-seven tenthousandths Course 1 ...
Pulsed Accretion in the Young Binary &
... these have been identified as possible sites for the study of early stellar evolution and planetary formation. Stellar formation starts when a gravitational collapse is triggered in dense regions of slowly rotating gaseous clouds. As the gravitational force depends on the inverse-square of the dista ...
... these have been identified as possible sites for the study of early stellar evolution and planetary formation. Stellar formation starts when a gravitational collapse is triggered in dense regions of slowly rotating gaseous clouds. As the gravitational force depends on the inverse-square of the dista ...
instructor notes: weeks 9/10
... bluer in colour than isolated galaxies, presumably because of the presence of recently-created hot young stars. It is believed that a tidal interaction with another galaxy has induced star formation, although the resulting excess luminosity is hidden behind obscuring clouds of gas and dust. Such gal ...
... bluer in colour than isolated galaxies, presumably because of the presence of recently-created hot young stars. It is believed that a tidal interaction with another galaxy has induced star formation, although the resulting excess luminosity is hidden behind obscuring clouds of gas and dust. Such gal ...
365 days of SKYWATCHING
... Unlike a star chart, Moon feature instructions are based on lunar topography and not our Earthly cardinal directions. While these pages outline what features should be visible on any given night, the position of the terminator may be slightly different for viewers in various time zones. Let’s start ...
... Unlike a star chart, Moon feature instructions are based on lunar topography and not our Earthly cardinal directions. While these pages outline what features should be visible on any given night, the position of the terminator may be slightly different for viewers in various time zones. Let’s start ...
Spectroscopic Atlas for Amateur Astronomers
... which systematically covers the classes O, B, A, F, G, K, M, by commenting most of the lines, visible in a medium resolved spectral profile was still missing. In the Internet we find many professional papers, mostly focused on small sections of a spectral profile. Nevertheless, they often contribute ...
... which systematically covers the classes O, B, A, F, G, K, M, by commenting most of the lines, visible in a medium resolved spectral profile was still missing. In the Internet we find many professional papers, mostly focused on small sections of a spectral profile. Nevertheless, they often contribute ...
The Milky Way - The Independent School
... Our Milky Way Galaxy is only one of the many billions of galaxies visible in the sky. This chapter will expand your horizon to discuss the different kinds of galaxies and their complex histories. Here you can expect ...
... Our Milky Way Galaxy is only one of the many billions of galaxies visible in the sky. This chapter will expand your horizon to discuss the different kinds of galaxies and their complex histories. Here you can expect ...
Ages of Young Stars
... Table 1: LDB ages compared with ages determined from upper main sequence fitting using models both with and without convective overshoot. Columns 2-4 list the apparent I magnitude of the LDB, the published LDB age and the source paper. Columns 5 and 6 give a bolometric magnitude and LDB age that hav ...
... Table 1: LDB ages compared with ages determined from upper main sequence fitting using models both with and without convective overshoot. Columns 2-4 list the apparent I magnitude of the LDB, the published LDB age and the source paper. Columns 5 and 6 give a bolometric magnitude and LDB age that hav ...
Ages of young stars
... are combinations of theoretical uncertainties and observational uncertainties associated with estimating the luminosity of the LDB. Contributing to the latter are distance estimates, reddening and bolometric corrections (for stellar luminosity not in the band observed), but these are usually small c ...
... are combinations of theoretical uncertainties and observational uncertainties associated with estimating the luminosity of the LDB. Contributing to the latter are distance estimates, reddening and bolometric corrections (for stellar luminosity not in the band observed), but these are usually small c ...
PH607lec08
... kinematic signatures of barred potentials have been used to infer their presence in some edge-on systems. What is noteworthy is that such edgeon bars appear to be associated with boxy or peanut-shaped bulges. ...
... kinematic signatures of barred potentials have been used to infer their presence in some edge-on systems. What is noteworthy is that such edgeon bars appear to be associated with boxy or peanut-shaped bulges. ...
Physical Properties of the Gas and Dust in the Orion B Molecular
... stars in the Orion association (Anthony-Twarog 1982). Earlier reviews about the Orion complex can be found in Goudis (1982), Maddalena et al. (1986), Genzel & Stutzki (1989), and Lada et al. (1993). The large-scale gas distribution of the Orion region has been mapped in 12 CO by Kutner et al. (1977) ...
... stars in the Orion association (Anthony-Twarog 1982). Earlier reviews about the Orion complex can be found in Goudis (1982), Maddalena et al. (1986), Genzel & Stutzki (1989), and Lada et al. (1993). The large-scale gas distribution of the Orion region has been mapped in 12 CO by Kutner et al. (1977) ...
exoplanet observing for amateurs
... camera lens attached to an astronomer’s CDD, monitors a set of star fields for several months before moving on to another set of star fields. When a star appears to fade by a small amount for a short time (e.g., <0.030 magnitude for ~3 hours), and when these fading events occur at regular intervals ...
... camera lens attached to an astronomer’s CDD, monitors a set of star fields for several months before moving on to another set of star fields. When a star appears to fade by a small amount for a short time (e.g., <0.030 magnitude for ~3 hours), and when these fading events occur at regular intervals ...
Chemical composition of 90 F and G disk dwarfs
... kinematics of disk stars, but substantial dispersions imposed on weak statistical trends. (2) There exists a real scatter in the run of [α/Fe] vs. [Fe/H] possibly due to the mixture of stars with different origins. The scatter seems to increase with decreasing metallicity starting at [Fe/H] ' −0.4. ...
... kinematics of disk stars, but substantial dispersions imposed on weak statistical trends. (2) There exists a real scatter in the run of [α/Fe] vs. [Fe/H] possibly due to the mixture of stars with different origins. The scatter seems to increase with decreasing metallicity starting at [Fe/H] ' −0.4. ...
Altair -- the ``hottest`` magnetically active star in X-rays
... type of A7 IV-V is a well-studied, optically bright star (V = 0.77, B − V = 0.22) with a mass of 1.8 M and an age of about 1.2 Gyr (Lachaume et al. 1999; Domiciano de Souza et al. 2005). It is the earliest and therefore hottest, magnetically active, single late-type main sequence star detected by t ...
... type of A7 IV-V is a well-studied, optically bright star (V = 0.77, B − V = 0.22) with a mass of 1.8 M and an age of about 1.2 Gyr (Lachaume et al. 1999; Domiciano de Souza et al. 2005). It is the earliest and therefore hottest, magnetically active, single late-type main sequence star detected by t ...
Luminosities and mass-loss rates of SMC and LMC AGB stars and
... 86 M-stars. Tables 1 and 2 list basic information: some common names (as listed by SIMBAD), an OGLE-iii identifier when this lightcurve is analysed and shown in Fig. 3, R.A. and declination in decimal degrees, the identifier used in figures and tables below, the adopted pulsation period, the (semi-) ...
... 86 M-stars. Tables 1 and 2 list basic information: some common names (as listed by SIMBAD), an OGLE-iii identifier when this lightcurve is analysed and shown in Fig. 3, R.A. and declination in decimal degrees, the identifier used in figures and tables below, the adopted pulsation period, the (semi-) ...
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.