Isotopic composition of Hg and Pt in 5 slowly rotating HgMn stars *
... neither extreme overabundances of rare earths, nor signicant overabundances of Si. Their spectral lines do not show conspicuous intensity variations. Neither have strong Send oprint requests to : G. Mathys ? Based on observations obtained at the European Southern Observatory, La Silla, Chile (ESO ...
... neither extreme overabundances of rare earths, nor signicant overabundances of Si. Their spectral lines do not show conspicuous intensity variations. Neither have strong Send oprint requests to : G. Mathys ? Based on observations obtained at the European Southern Observatory, La Silla, Chile (ESO ...
Astronomy Assignment #1
... 4. During a night, how do the stars move? What angle does their nightly path make with respect to the horizon? How does it depend on latitude? During the course of a night the stars appear to move westward, rising somewhere along the eastern horizon (except for the circumpolar stars that never rise ...
... 4. During a night, how do the stars move? What angle does their nightly path make with respect to the horizon? How does it depend on latitude? During the course of a night the stars appear to move westward, rising somewhere along the eastern horizon (except for the circumpolar stars that never rise ...
Solutions
... 4. During a night, how do the stars move? What angle does their nightly path make with respect to the horizon? How does it depend on latitude? During the course of a night the stars appear to move westward, rising somewhere along the eastern horizon (except for the circumpolar stars that never rise ...
... 4. During a night, how do the stars move? What angle does their nightly path make with respect to the horizon? How does it depend on latitude? During the course of a night the stars appear to move westward, rising somewhere along the eastern horizon (except for the circumpolar stars that never rise ...
Module 11.1.1: Galaxies: Morphology and the Hubble Sequence
... of those. And those are sort of the last pre-‐modern compilations of galaxian data. Nowadays, it's all done in fully automated objective fashion from digital sky surveys, and modern catalogs of ...
... of those. And those are sort of the last pre-‐modern compilations of galaxian data. Nowadays, it's all done in fully automated objective fashion from digital sky surveys, and modern catalogs of ...
Chapter 15 Stars, Galaxies, and Universe
... •Spiral arms contain new stars, gas, dust •New stars formed in spiral arms •Elliptical – round or oval shape, billions of stars, little gas or dust, therefore old stars •Irregular – smaller than other galaxies •Young stars, lots of gas and dust •Located close to larger galaxies. ...
... •Spiral arms contain new stars, gas, dust •New stars formed in spiral arms •Elliptical – round or oval shape, billions of stars, little gas or dust, therefore old stars •Irregular – smaller than other galaxies •Young stars, lots of gas and dust •Located close to larger galaxies. ...
Starburst Galaxies - Beck-Shop
... region, which is a gaseous nebula with an emission-line spectrum (Box 2.2). H II regions are some of the most spectacular sights in the sky – rivalling galaxies – and the well-known Orion Nebula (M 42, Fig. 2.1) is exactly just such a region that has developed on the nearest side to us of the Orion ...
... region, which is a gaseous nebula with an emission-line spectrum (Box 2.2). H II regions are some of the most spectacular sights in the sky – rivalling galaxies – and the well-known Orion Nebula (M 42, Fig. 2.1) is exactly just such a region that has developed on the nearest side to us of the Orion ...
ppt
... dispersion for 10-point averages. For most objects, the dispersion of 10point averages is much higher than that which is expected for white noise, especially for brighter magnitudes. The dotted line shows the expected dispersion of the 10-point means according to the discussion in this paper, with a ...
... dispersion for 10-point averages. For most objects, the dispersion of 10point averages is much higher than that which is expected for white noise, especially for brighter magnitudes. The dotted line shows the expected dispersion of the 10-point means according to the discussion in this paper, with a ...
Galaxy Sorting
... galaxies contain mostly old stars, with very little gas and dust found between stars. Since new stars form from clouds of interstellar gas and dust, elliptical galaxies lack the raw ingredients to make new stars. Spiral galaxies, on the other hand, have a mix of young and old stars. Interstellar ...
... galaxies contain mostly old stars, with very little gas and dust found between stars. Since new stars form from clouds of interstellar gas and dust, elliptical galaxies lack the raw ingredients to make new stars. Spiral galaxies, on the other hand, have a mix of young and old stars. Interstellar ...
Lecture 3 - University of Washington
... use HST/WFC3 imaging from the CANDELS Multicycle Treasury Survey, in conjunction with the Sloan Digital Sky Survey, to explore the evolution of galactic structure for galaxies with stellar masses > 3e10 Msun from z = 2.2 to the present epoch, a time span of 10 Gyr. We explore the relationship betwee ...
... use HST/WFC3 imaging from the CANDELS Multicycle Treasury Survey, in conjunction with the Sloan Digital Sky Survey, to explore the evolution of galactic structure for galaxies with stellar masses > 3e10 Msun from z = 2.2 to the present epoch, a time span of 10 Gyr. We explore the relationship betwee ...
The cosmological significance of high
... investigations of its stellar content. The H I mass of the cloud is 2.0 × 107 (d/27 kpc)2 M⊙ , making Complex H one of the most massive HVCs if its distance is more than ∼ 20 kpc. Virtually all similar H I clouds in other galaxy groups are associated with low surface brightness dwarf galaxies. We se ...
... investigations of its stellar content. The H I mass of the cloud is 2.0 × 107 (d/27 kpc)2 M⊙ , making Complex H one of the most massive HVCs if its distance is more than ∼ 20 kpc. Virtually all similar H I clouds in other galaxy groups are associated with low surface brightness dwarf galaxies. We se ...
ASPEN WORKSHOP 2003
... WARNING: These notes were not reviewed by the speakers. For more reliable summaries of what they said (without my editorializing), you should ask the individual speakers for their Powerpoint presentations. Also, notes for several talks are missing since I did not have a working laptop for them and h ...
... WARNING: These notes were not reviewed by the speakers. For more reliable summaries of what they said (without my editorializing), you should ask the individual speakers for their Powerpoint presentations. Also, notes for several talks are missing since I did not have a working laptop for them and h ...
Navigation: The Mariner`s Quadrant
... edges for sighting. The only scale needed was the degree marks on the curved edge. It was light and easy to handle. ...
... edges for sighting. The only scale needed was the degree marks on the curved edge. It was light and easy to handle. ...
Learn to write, compare, and order decimals using place value and
... Additional Example 1A & B: Reading and Writing Decimals Write each decimal in standard form, expanded form, and words. ...
... Additional Example 1A & B: Reading and Writing Decimals Write each decimal in standard form, expanded form, and words. ...
The Final Version of the White Paper is available.
... The discovery almost 20 years ago of the first giant planet outside of the solar system (Mayor & Queloz 1995) spawned a real revolution in astronomy. The completely unexpected characteristics of this first planet captured the imagination and interest of the scientific community and the general publi ...
... The discovery almost 20 years ago of the first giant planet outside of the solar system (Mayor & Queloz 1995) spawned a real revolution in astronomy. The completely unexpected characteristics of this first planet captured the imagination and interest of the scientific community and the general publi ...
A Digital Spectral Classification Atlas
... The MK Spectral classification system was founded by W.W. Morgan and P.C. Keenan in the year 1943, with the publication of the first photographic spectral classification atlas, An Atlas of Stellar Spectra (Morgan, Keenan & Kelleman, 1943). Since that time, the MK system has been extensively revised ...
... The MK Spectral classification system was founded by W.W. Morgan and P.C. Keenan in the year 1943, with the publication of the first photographic spectral classification atlas, An Atlas of Stellar Spectra (Morgan, Keenan & Kelleman, 1943). Since that time, the MK system has been extensively revised ...
Edwin Hubble (1889
... weather permitted and in the last five months have netted nine novae and two variables." ...
... weather permitted and in the last five months have netted nine novae and two variables." ...
Parallax
... Of course astronomers are not ones to use simple methods. They have goobered up this measurement just like the ones with magnitude. So keep reading and the enumeration as to how astronomers use parallax to measure the distance to a star will be given. Except for our sun, the stars are pretty far aw ...
... Of course astronomers are not ones to use simple methods. They have goobered up this measurement just like the ones with magnitude. So keep reading and the enumeration as to how astronomers use parallax to measure the distance to a star will be given. Except for our sun, the stars are pretty far aw ...
ALFALFA H-alpha: The Star-Formation-Rate Density
... Over one hundred billion stars lie in the Milky Way galaxy, a moderate-sized galaxy in a universe of roughly one hundred billion galaxies. These galaxies thus amount to 1022 (ten sextillion) stars in our Universe. The science of astronomy allows us to contemplate such grand numbers and to investigat ...
... Over one hundred billion stars lie in the Milky Way galaxy, a moderate-sized galaxy in a universe of roughly one hundred billion galaxies. These galaxies thus amount to 1022 (ten sextillion) stars in our Universe. The science of astronomy allows us to contemplate such grand numbers and to investigat ...
Lecture 9: The interstellar medium (ISM)
... • Number along a given lines of sight in glactic plane ~ 7 or 8/kpc • Typical size a few pc to a few tens of parsecs • Typical mass MHI ~ 100 M⊙ • Temperature T ~ 90 K • Radio emission λ = 21 cm, frequency f = 1420.406 MHz ...
... • Number along a given lines of sight in glactic plane ~ 7 or 8/kpc • Typical size a few pc to a few tens of parsecs • Typical mass MHI ~ 100 M⊙ • Temperature T ~ 90 K • Radio emission λ = 21 cm, frequency f = 1420.406 MHz ...
The Birth Environment of the Solar System
... photons) provides ionization, which can influence both the early star formation process and the subsequent evolution of our circumstellar disk. [3] The presence of short-lived radioactive species inferred from meteorites provides another class of constraints. Radioactive nuclei can be produced in su ...
... photons) provides ionization, which can influence both the early star formation process and the subsequent evolution of our circumstellar disk. [3] The presence of short-lived radioactive species inferred from meteorites provides another class of constraints. Radioactive nuclei can be produced in su ...
Effect of the stellar spin history on the tidal evolution of close
... been detected (Benedict et al. 1998; Kiraga & Stepien 2007; Charbonneau et al. 2009). In contrast to Sun-like stars that are mostly radiative except for a small (in terms of mass) convective region at the surface, very low-mass stars (M∗ < 0.35 M ) are entirely convective (Chabrier & Baraffe 1997). ...
... been detected (Benedict et al. 1998; Kiraga & Stepien 2007; Charbonneau et al. 2009). In contrast to Sun-like stars that are mostly radiative except for a small (in terms of mass) convective region at the surface, very low-mass stars (M∗ < 0.35 M ) are entirely convective (Chabrier & Baraffe 1997). ...
Marking Scheme of Observational Sessions
... mark every report and SELECT 8 REPORTS THAT HAVE HIGEST MARKS to enter to the marks list. If the observer will be drawn deep sky objects such as ( Nebulas, Galaxies, Messier objects in the constellation mapping area, Give MINUS MARKS for that. ( drawing those objects inside constellation mapping are ...
... mark every report and SELECT 8 REPORTS THAT HAVE HIGEST MARKS to enter to the marks list. If the observer will be drawn deep sky objects such as ( Nebulas, Galaxies, Messier objects in the constellation mapping area, Give MINUS MARKS for that. ( drawing those objects inside constellation mapping are ...
Discovery of extremely lead-rich subdwarfs: does heavy metal signal
... Hot subdwarfs represent a group of low-mass helium-burning stars formed through binarystar interactions and include some of the most chemically peculiar stars in the Galaxy. Stellar evolution theory suggests that they should have helium-rich atmospheres but, because radiation causes hydrogen to diff ...
... Hot subdwarfs represent a group of low-mass helium-burning stars formed through binarystar interactions and include some of the most chemically peculiar stars in the Galaxy. Stellar evolution theory suggests that they should have helium-rich atmospheres but, because radiation causes hydrogen to diff ...
... as RRc in the GCVS (Kholopov et al. 1987) with a period of 0.28779276 d. Until 1977 it was included in photometric programmes of RRL stars (e.g., Bookmeyer et al. 1977). The star is declared as an RRL in the SIMBAD data base. These facts perhaps led Peña et al. (2012) to include the star in their p ...
Perseus (constellation)
Perseus, named after the Greek mythological hero Perseus, is a constellation in the northern sky. It was one of 48 listed by the 2nd-century astronomer Ptolemy and among the 88 modern constellations defined by the International Astronomical Union (IAU). It is located in the northern celestial hemisphere near several other constellations named after legends surrounding Perseus, including Andromeda to the west and Cassiopeia to the north. Perseus is also bordered by Aries and Taurus to the south, Auriga to the east, Camelopardalis to the north, and Triangulum to the west.The galactic plane of the Milky Way passes through Perseus but is mostly obscured by molecular clouds. The constellation's brightest star is the yellow-white supergiant Alpha Persei (also called Mirfak), which shines at magnitude 1.79. It and many of the surrounding stars are members of an open cluster known as the Alpha Persei Cluster. The best-known star, however, is Algol (Beta Persei), linked with ominous legends because of its variability, which is noticeable to the naked eye. Rather than being an intrinsically variable star, it is an eclipsing binary. Other notable star systems in Perseus include X Persei, a binary system containing a neutron star, and GK Persei, a nova that peaked at magnitude 0.2 in 1901. The Double Cluster, comprising two open clusters quite near each other in the sky, was known to the ancient Chinese. The constellation gives its name to the Perseus Cluster (Abell 426), a massive galaxy cluster located 250 million light-years from Earth. It hosts the radiant of the annual Perseids meteor shower—one of the most prominent meteor showers in the sky.