DoAr21_AAS2005 - Astronomy at Swarthmore College
... Weak-lined T Tauri Star (WTTS), having shown H-alpha in emission in the 1950s but without H-alpha emission reported subsequently and without a strong IR excess. It is only about 1 Myr old (left) and has already been identified, via lowresolution x-ray spectroscopy, to have strong, hard, and variable ...
... Weak-lined T Tauri Star (WTTS), having shown H-alpha in emission in the 1950s but without H-alpha emission reported subsequently and without a strong IR excess. It is only about 1 Myr old (left) and has already been identified, via lowresolution x-ray spectroscopy, to have strong, hard, and variable ...
![arXiv:1705.00964v1 [astro-ph.GA] 2 May 2017](http://s1.studyres.com/store/data/013011793_1-8f89fb3e8b5cd5cf78613aebb3c8e2a5-300x300.png)
arXiv:1705.00964v1 [astro-ph.GA] 2 May 2017
... J1819+3845 might be related to the foreground, bright star Vega. We therefore examined whether ionized gas associated with foreground stars provides a good explanation for the IDV phenomenon. Although we continue to monitor PKS1322-110, it will be some time before that data set rivals the coverage o ...
... J1819+3845 might be related to the foreground, bright star Vega. We therefore examined whether ionized gas associated with foreground stars provides a good explanation for the IDV phenomenon. Although we continue to monitor PKS1322-110, it will be some time before that data set rivals the coverage o ...
The Physics of Energy sources Stellar fusion
... ! Could you explain what is the source of energy of a Star? ! What is the proton-proton chain? ! Why can it work? ! What is the slowest process in this chain? ...
... ! Could you explain what is the source of energy of a Star? ! What is the proton-proton chain? ! Why can it work? ! What is the slowest process in this chain? ...
HR Diagram of Messier 80 using Hubble Space Telescope Data
... Go to http://hla.stsci.edu/ Click “Enter Site.” Search for M80. Then do an “Advanced Search”. Check off only the WFPC2 instrument. Search for Proposal ID 11233. Two “visits” come up, and eight results appear. Six of these results are not relevant to this lab. You only want to use “visit 6” for this ...
... Go to http://hla.stsci.edu/ Click “Enter Site.” Search for M80. Then do an “Advanced Search”. Check off only the WFPC2 instrument. Search for Proposal ID 11233. Two “visits” come up, and eight results appear. Six of these results are not relevant to this lab. You only want to use “visit 6” for this ...
Stars and Galaxies
... Sine of the parallax (angle) x Earth’s distance to the Sun = Distance to the star The angles involved for strellar observations are very small and difficult to measure. Proxima Centauri, has a parallax of 0.77 arcsec. This angle is approximately the angle subtended by an object about 2 centimete ...
... Sine of the parallax (angle) x Earth’s distance to the Sun = Distance to the star The angles involved for strellar observations are very small and difficult to measure. Proxima Centauri, has a parallax of 0.77 arcsec. This angle is approximately the angle subtended by an object about 2 centimete ...
Turning over a new leaf
... waves like brown dwarf LP944-20, described on page 338 of this issue by Berger and colleagues2. This nearby brown dwarf (some 15 light years away) appears to be emitting a constant background of radio waves at a wavelength of 3.6 cm. These occasionally flare up for a few hours, growing in strength b ...
... waves like brown dwarf LP944-20, described on page 338 of this issue by Berger and colleagues2. This nearby brown dwarf (some 15 light years away) appears to be emitting a constant background of radio waves at a wavelength of 3.6 cm. These occasionally flare up for a few hours, growing in strength b ...
Neon abundances - UCL Astrophysics Group
... from marginal deficits of 0.1±0.3 dex to underabundances of an order of magnitude or more. In many cases, the lines are so weak that only upper limits can be established. The most extreme example found is y Her with an underabundance of at least 1.5 dex. These underabundances are qualitatively expec ...
... from marginal deficits of 0.1±0.3 dex to underabundances of an order of magnitude or more. In many cases, the lines are so weak that only upper limits can be established. The most extreme example found is y Her with an underabundance of at least 1.5 dex. These underabundances are qualitatively expec ...
Kepler-452b is not a new Earth A twin of the Sun
... materials available through this course may be made, solely for personal, noncommercial use. Users may not distribute such copies to others, whether or not in electronic form, whether or not for a charge or other consideration, without prior written consent of the copyright holder of the materials. ...
... materials available through this course may be made, solely for personal, noncommercial use. Users may not distribute such copies to others, whether or not in electronic form, whether or not for a charge or other consideration, without prior written consent of the copyright holder of the materials. ...
Supermassive Black Holes in Inactive Galaxies Encyclopedia of Astronomy & Astrophysics eaa.iop.org
... holes (BHs) that accrete gas and stars and so transform gravitational potential energy into radiation. Expected BH masses are M• ~ 106–109.5M⊙. A wide array of phenomena can be understood within this picture. However, the subject has had an outstanding problem: there was no dynamical evidence that B ...
... holes (BHs) that accrete gas and stars and so transform gravitational potential energy into radiation. Expected BH masses are M• ~ 106–109.5M⊙. A wide array of phenomena can be understood within this picture. However, the subject has had an outstanding problem: there was no dynamical evidence that B ...
Properties of Wolf-Rayet Stars - Paul Crowther, University of Sheffield
... include improved Milky Way statistics from near-IR surveys, different flavours of hydrogen-rich and hydrogen-poor WN stars, WR masses from binary orbits, plus spectroscopic analysis of WR stars resulting in stellar temperatures, luminosities, ionizing fluxes, plus wind properties accounting for clum ...
... include improved Milky Way statistics from near-IR surveys, different flavours of hydrogen-rich and hydrogen-poor WN stars, WR masses from binary orbits, plus spectroscopic analysis of WR stars resulting in stellar temperatures, luminosities, ionizing fluxes, plus wind properties accounting for clum ...
The Primordial Abundance of $^ 6$ Li and $^ 9$ be
... both possibilities in the discussion which follows. Our Z = 10−4 isochrone corresponds to [Fe/H] = −2.55 and [α/Fe] = +0.40 (assuming that the effects of α-element enhancement may be accounted for by modifying the overall Z of the star, as outlined by Salaris, Chieffi & Straniero 1993) and so is the ...
... both possibilities in the discussion which follows. Our Z = 10−4 isochrone corresponds to [Fe/H] = −2.55 and [α/Fe] = +0.40 (assuming that the effects of α-element enhancement may be accounted for by modifying the overall Z of the star, as outlined by Salaris, Chieffi & Straniero 1993) and so is the ...
Chapter 26: Stars, Galaxies, and the Universe Stars
... on the main sequence for ―only‖ 10 million years or so. Very small stars may be main sequence stars for tens to hundreds of billions of years. Red Giants and White Dwarfs As a star begins to use up its hydrogen, it then begins to fuse helium atoms together into heavier atoms like carbon. Eventually, ...
... on the main sequence for ―only‖ 10 million years or so. Very small stars may be main sequence stars for tens to hundreds of billions of years. Red Giants and White Dwarfs As a star begins to use up its hydrogen, it then begins to fuse helium atoms together into heavier atoms like carbon. Eventually, ...
20 – N10/4/PHYSI/SP3/ENG/TZ0/XX Option E
... (b) Explain how the future of the universe may be predicted by comparing the estimated density of the universe to the critical density. ...
... (b) Explain how the future of the universe may be predicted by comparing the estimated density of the universe to the critical density. ...
What is a white dwarf?
... Einstein’s theory of relativity says that nothing can move faster than light. [The speed of limit is the same relative to all observers.] When electron speeds in a white dwarf approach the speed of light, electron degeneracy pressure can no longer support the white dwarf. ...
... Einstein’s theory of relativity says that nothing can move faster than light. [The speed of limit is the same relative to all observers.] When electron speeds in a white dwarf approach the speed of light, electron degeneracy pressure can no longer support the white dwarf. ...
A Question of Planets - Vanderbilt University
... that their brightness varies dramatically. More recently astronomers have been studying them because they can provide important insights into how the Sun and solar system evolved. Twenty years ago, scientists thought that T Tauri stars had extremely strong solar winds blowing outward at velocities o ...
... that their brightness varies dramatically. More recently astronomers have been studying them because they can provide important insights into how the Sun and solar system evolved. Twenty years ago, scientists thought that T Tauri stars had extremely strong solar winds blowing outward at velocities o ...
Sun, Moon, Earth,
... – Neutron Stars: Forms from the remains of the old star. • Very very high density and very very small. – As much as three times the mass of our star in an area the size of a city. – Some give off regular pulses of radio waves and are called pulsars. (these were originally called LGMs). ...
... – Neutron Stars: Forms from the remains of the old star. • Very very high density and very very small. – As much as three times the mass of our star in an area the size of a city. – Some give off regular pulses of radio waves and are called pulsars. (these were originally called LGMs). ...
phys-1600 - Dave Heppenstall
... • In Io's case, there are immense volcanoes which are constantly being churned inside out and renewing its surface. This is due to the close proximity to Jupiter and the enormous gravitational force. • Io has no atmosphere. If Io moves in closer to Jupiter, it could be torn apart. Io is also in an e ...
... • In Io's case, there are immense volcanoes which are constantly being churned inside out and renewing its surface. This is due to the close proximity to Jupiter and the enormous gravitational force. • Io has no atmosphere. If Io moves in closer to Jupiter, it could be torn apart. Io is also in an e ...
PH607lec10-4gal2
... No two galaxies have the same star formation history Dwarfs do not contain dark matter…..however, unusually: Dwarf Spheroidal, Leo I : ...
... No two galaxies have the same star formation history Dwarfs do not contain dark matter…..however, unusually: Dwarf Spheroidal, Leo I : ...
Metal-poor Stars
... and evolution of the elements and the involved nucleosynthesis processes. This knowledge is invaluable for our understanding of the cosmic chemical evolution and the onset of star- and galaxy formation. Metal-poor stars are the local equivalent of the high-redshift Universe. Hence, they also provide ...
... and evolution of the elements and the involved nucleosynthesis processes. This knowledge is invaluable for our understanding of the cosmic chemical evolution and the onset of star- and galaxy formation. Metal-poor stars are the local equivalent of the high-redshift Universe. Hence, they also provide ...
Stellar kinematics
Stellar kinematics is the study of the movement of stars without needing to understand how they acquired their motion. This differs from stellar dynamics, which takes into account gravitational effects. The motion of a star relative to the Sun can provide useful information about the origin and age of a star, as well as the structure and evolution of the surrounding part of the Milky Way.In astronomy, it is widely accepted that most stars are born within molecular clouds known as stellar nurseries. The stars formed within such a cloud compose open clusters containing dozens to thousands of members. These clusters dissociate over time. Stars that separate themselves from the cluster's core are designated as members of the cluster's stellar association. If the remnant later drifts through the Milky Way as a coherent assemblage, then it is termed a moving group.