Potassium abundances in nearby metal-poor stars
... of potassium abundances is difficult. Only the resonance doublet (K 7665 and 7699 Å) is available for abundance analyses of metal-poor stars, however, K resonance lines are often blended with very strong telluric O2 lines. There have been only a few studies which attempted to investigate the stell ...
... of potassium abundances is difficult. Only the resonance doublet (K 7665 and 7699 Å) is available for abundance analyses of metal-poor stars, however, K resonance lines are often blended with very strong telluric O2 lines. There have been only a few studies which attempted to investigate the stell ...
Entering SH within Physics and Astronomy and Joint Degrees
... your adviser of studies at this stage, though the honours advisers may be contacted should you wish. For students on degree programmes wholly within the School the SH adviser is currently Dr Natalia Korolkova. The School’s Director of Teaching, Dr Bruce Sinclair, is also willing to discuss matters w ...
... your adviser of studies at this stage, though the honours advisers may be contacted should you wish. For students on degree programmes wholly within the School the SH adviser is currently Dr Natalia Korolkova. The School’s Director of Teaching, Dr Bruce Sinclair, is also willing to discuss matters w ...
The 8190-A sodium doublet in cataclysmic variables
... both nights. Using the single spectrum taken on night 1, which was on the rise to outburst, we derive a spectral type for the secondary of between M5 and M6, much later than suggested by Mateo et al. (1985). Given that the orbital period has been determined to be 4.33 h, if our estimate is correct, ...
... both nights. Using the single spectrum taken on night 1, which was on the rise to outburst, we derive a spectral type for the secondary of between M5 and M6, much later than suggested by Mateo et al. (1985). Given that the orbital period has been determined to be 4.33 h, if our estimate is correct, ...
Paper 3 (pdf)
... papers in 20 years, over 5% of all papers ever written about AGN. Thus, the extra information from polarimetric observations has provided a fundamental contribution to the understanding of AGN. Although tens of thousands of X-ray sources are known from the ROSAT all-sky survey, polarization studies ...
... papers in 20 years, over 5% of all papers ever written about AGN. Thus, the extra information from polarimetric observations has provided a fundamental contribution to the understanding of AGN. Although tens of thousands of X-ray sources are known from the ROSAT all-sky survey, polarization studies ...
S.V. Berdyugina, I.G. Usoskin, Preferred Longitudes in Sunspot
... have been found to migrate in longitude as a rigid structure, seemingly due to the star’s differential rotation. This suggests that solar active longitudes, if they exist, may also follow the surface differential rotation, and the assumption on their even rotation made by previous investigators is pro ...
... have been found to migrate in longitude as a rigid structure, seemingly due to the star’s differential rotation. This suggests that solar active longitudes, if they exist, may also follow the surface differential rotation, and the assumption on their even rotation made by previous investigators is pro ...
Infrared Solar Physics - National Optical Astronomy Observatory
... “Why does anyone still observe the Sun using visible wavelengths of light?” a colleague recently asked of me. Certainly night-time astronomers have been exploiting the infrared spectrum for many years to address critical science questions in that field. The spatial resolution, flux and background pr ...
... “Why does anyone still observe the Sun using visible wavelengths of light?” a colleague recently asked of me. Certainly night-time astronomers have been exploiting the infrared spectrum for many years to address critical science questions in that field. The spatial resolution, flux and background pr ...
VLVNT_APP_Roadmaps_Ch_Spiering_
... further out into the Universe than possible with gamma-rays. Together with gammaray and cosmic ray observations (and with IceCube), it could pave the way to real multi-messenger astronomy. • However, in absence of established cosmic high-energy neutrino sources, it is difficult to assess the sensiti ...
... further out into the Universe than possible with gamma-rays. Together with gammaray and cosmic ray observations (and with IceCube), it could pave the way to real multi-messenger astronomy. • However, in absence of established cosmic high-energy neutrino sources, it is difficult to assess the sensiti ...
Richard Congdon. pdf
... Only a few of the elements in the universe were created at its beginning during the Big Bang, namely: hydrogen, deuterium, helium-3 and lithium (1H, 2H, 3He, 7Li). No further stable elements were created at this time because the rapid expansion and cooling, as the Universe expanded into of the void. ...
... Only a few of the elements in the universe were created at its beginning during the Big Bang, namely: hydrogen, deuterium, helium-3 and lithium (1H, 2H, 3He, 7Li). No further stable elements were created at this time because the rapid expansion and cooling, as the Universe expanded into of the void. ...
JHU Talk 1Feb05 - NRAO Charlottesville
... spectrum of planets, young stars, many distant galaxies. Cool objects tend to be extended, hence ALMA’s mandate to image with high sensitivity, recovering all of an object’s emitted flux at the frequency of interest. Most of the observed transitions of the 125 known interstellar molecules lie in the ...
... spectrum of planets, young stars, many distant galaxies. Cool objects tend to be extended, hence ALMA’s mandate to image with high sensitivity, recovering all of an object’s emitted flux at the frequency of interest. Most of the observed transitions of the 125 known interstellar molecules lie in the ...
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... The lightcurve is characterised by rapid aperiodic ‘flaring’ throughout the 16 years of observations. Changes in the high excitation emission line component of the spectrum imply evolution in the stellar temperature - as expected for luminous blue variables although somewhat surprisingly, spectrosco ...
... The lightcurve is characterised by rapid aperiodic ‘flaring’ throughout the 16 years of observations. Changes in the high excitation emission line component of the spectrum imply evolution in the stellar temperature - as expected for luminous blue variables although somewhat surprisingly, spectrosco ...
Five Years of Swift Science: GRBs and More!
... • Swift has delivered a remarkably successful science mission to date, powered by an innovative operations concept that has continued to evolve as driven by scientific interest • The latest changes will enable an even more responsive observatory, giving more GI monitoring and ToO responsiveness • Fo ...
... • Swift has delivered a remarkably successful science mission to date, powered by an innovative operations concept that has continued to evolve as driven by scientific interest • The latest changes will enable an even more responsive observatory, giving more GI monitoring and ToO responsiveness • Fo ...
VLT observations of GRS 1915+ 105
... Fig. 1. VLT low resolution spectra of GRS 1915+105 obtained on 1999 May 29 (before a radio outburst) and 1999 July 04 (during a radio outburst) using the SK filter with ISAAC. The emission line identifications are indicated. Å emission when in outburst. An interesting property of some emission line ...
... Fig. 1. VLT low resolution spectra of GRS 1915+105 obtained on 1999 May 29 (before a radio outburst) and 1999 July 04 (during a radio outburst) using the SK filter with ISAAC. The emission line identifications are indicated. Å emission when in outburst. An interesting property of some emission line ...
Chapter 7 Elliptical Galaxies Chapter 16 Elliptical Galaxies
... to the particles themselves or has further contributions from other sources. If the potential is only due to the particles described by f, then self-consistency is fulfilled: ...
... to the particles themselves or has further contributions from other sources. If the potential is only due to the particles described by f, then self-consistency is fulfilled: ...
Large distance of epsilon Aurigae from interstellar
... The long-period (P = 27.1 years) peculiar eclipsing binary ε Aur, which has recently completed its 2 year-long primary eclipse, has perplexed astronomers for over a century. The eclipse arises from the transit of a huge, cool and opaque, disk across the face of the F0 Iab star. One of the principal ...
... The long-period (P = 27.1 years) peculiar eclipsing binary ε Aur, which has recently completed its 2 year-long primary eclipse, has perplexed astronomers for over a century. The eclipse arises from the transit of a huge, cool and opaque, disk across the face of the F0 Iab star. One of the principal ...
Herbig-Haro jet in the Haro 6–10 system
... The integral spectrum of the object, obtained by summation of the spectra from each pupil with detectable continuum (Fig. 2a), is in good agreement with our echelle spectrum. Emission lines of Hα, [O i], [N ii] and [S ii] are prominent. Besides, the absorption line 6708 Å of Li i, typical for PMS s ...
... The integral spectrum of the object, obtained by summation of the spectra from each pupil with detectable continuum (Fig. 2a), is in good agreement with our echelle spectrum. Emission lines of Hα, [O i], [N ii] and [S ii] are prominent. Besides, the absorption line 6708 Å of Li i, typical for PMS s ...
WASHINGTON STATE UNIVERSITY - American Institute of Physics
... M.S. degree with a thesis, a minimum of 30 credits is required, of which 21 must be for graded courses. A minimum 3.0 GPA must be maintained. One academic year of residence is required. No foreign language is required. Must pass oral final examination. Students making normal progress toward a Ph.D. ...
... M.S. degree with a thesis, a minimum of 30 credits is required, of which 21 must be for graded courses. A minimum 3.0 GPA must be maintained. One academic year of residence is required. No foreign language is required. Must pass oral final examination. Students making normal progress toward a Ph.D. ...
Astronomy Astrophysics
... young solar analogues. The sample includes five single G0-G5V stars with ages between '130 Myr and 700 Myr: EK Dra, π1 UMa, HN Peg, k1 Cet and BE Cet. In this study we also include the Pleiades-age ('130 Myr) K0V star DX Leo. Our analysis is based on high precision photometric observations carried o ...
... young solar analogues. The sample includes five single G0-G5V stars with ages between '130 Myr and 700 Myr: EK Dra, π1 UMa, HN Peg, k1 Cet and BE Cet. In this study we also include the Pleiades-age ('130 Myr) K0V star DX Leo. Our analysis is based on high precision photometric observations carried o ...
Abstracts - New Frontiers in Black Hole Astrophysics
... birthdays join the first 50-year-old plausible design for a gravitational radiation detector. Remarkable progress was made in General Relativity in the years 1916-1918 (Lense, Thirring, Reisner, Nordstrom, and others) despite the ongoing Great War. And even an unrecognized GRB hit a nuclear test mon ...
... birthdays join the first 50-year-old plausible design for a gravitational radiation detector. Remarkable progress was made in General Relativity in the years 1916-1918 (Lense, Thirring, Reisner, Nordstrom, and others) despite the ongoing Great War. And even an unrecognized GRB hit a nuclear test mon ...
Symbiotic Stars as Laboratories for the Study of
... outbursts, jets, and accretion disks in symbiotic stars. 1. Introduction: What are symbiotic stars? Symbiotic stars are interacting binary stars in which a hot white dwarf (WD; or in a few cases a main-sequence star) orbits a red-giant star and captures material from the wind of the red giant (RG). ...
... outbursts, jets, and accretion disks in symbiotic stars. 1. Introduction: What are symbiotic stars? Symbiotic stars are interacting binary stars in which a hot white dwarf (WD; or in a few cases a main-sequence star) orbits a red-giant star and captures material from the wind of the red giant (RG). ...
Booklet - Centrum Astronomiczne im. M.Kopernika PAN
... Pulsational light variability in Carbon-rich post-AGB stars in the Milky Way Galaxy and the Magellanic Clouds B. Hrivnak, Valparaiso University, USA We recently published the results of a long-term photometric monitoring program of 12 carbon-rich postAGB stars in the Milky Way Galaxy. These objects ...
... Pulsational light variability in Carbon-rich post-AGB stars in the Milky Way Galaxy and the Magellanic Clouds B. Hrivnak, Valparaiso University, USA We recently published the results of a long-term photometric monitoring program of 12 carbon-rich postAGB stars in the Milky Way Galaxy. These objects ...
Science Book - Chapter 1: Introduction
... Plans for the “6-meter class” DMT wide field telescope and camera were presented at a workshop on gravity at SLAC National Accelerator Laboratory in August 1998 (Tyson 1998). The science case for such a telescope was submitted to the 2000 Astronomy and Astrophysics Decadal Survey in June 1999. That ...
... Plans for the “6-meter class” DMT wide field telescope and camera were presented at a workshop on gravity at SLAC National Accelerator Laboratory in August 1998 (Tyson 1998). The science case for such a telescope was submitted to the 2000 Astronomy and Astrophysics Decadal Survey in June 1999. That ...
Further VLBA Observations of SiO Masers toward Mira
... cooler region at 3–5 R? where the (silicate) dust forms; see Reid & Menten (1997), Danchi et al. (1994). Circumstellar SiO masers tend to occur in clumpy, partial rings centered on the central star (Diamond et al. 1994). This is presumed to be due to the longer paths through constant velocity gas ne ...
... cooler region at 3–5 R? where the (silicate) dust forms; see Reid & Menten (1997), Danchi et al. (1994). Circumstellar SiO masers tend to occur in clumpy, partial rings centered on the central star (Diamond et al. 1994). This is presumed to be due to the longer paths through constant velocity gas ne ...
Indian Institute of Astrophysics
The Indian Institute of Astrophysics (IIA), with its headquarters in Bangalore (Karnataka state), India, is a premier national institute of India for the study of and research into topics pertaining to astronomy, astrophysics and related subjects.The Institute has a network of laboratories and observatories located in various places in India, including Kodaikanal (the Kodaikanal Solar Observatory), Kavalur (the Vainu Bappu Observatory), Gauribidanur, Hanle (the Indian Astronomical Observatory) and Hosakote.