The old globular cluster system of the dIrr galaxy NGC 1427A in the
... (2000) and Harris (2003). In all these models, the GCSs of low-mass dwarf galaxies, the most numerous galaxy type in galaxy clusters (Sandage 2005, and references therein), are envisioned as the building blocks of the GCSs of the more massive galaxies. At present the role of the GCSs of dIrr galaxie ...
... (2000) and Harris (2003). In all these models, the GCSs of low-mass dwarf galaxies, the most numerous galaxy type in galaxy clusters (Sandage 2005, and references therein), are envisioned as the building blocks of the GCSs of the more massive galaxies. At present the role of the GCSs of dIrr galaxie ...
The CCD Photometric Calibration Cookbook
... CCD (Charge-Coupled Device) photometric calibration is concerned with converting the arbitrary units in which CCD images are recorded into standard, reproducible units. In principle the observed brightness could be calibrated into genuine physical units, such as W m , and indeed this is occasionally ...
... CCD (Charge-Coupled Device) photometric calibration is concerned with converting the arbitrary units in which CCD images are recorded into standard, reproducible units. In principle the observed brightness could be calibrated into genuine physical units, such as W m , and indeed this is occasionally ...
An X-Ray, Optical and Infra-red study of High-Mass X
... AN X-RAY, OPTICAL AND INFRA-RED STUDY OF HIGH-MASS X-RAY BINARIES IN THE SMALL MAGELLANIC CLOUD by Lee John Townsend ...
... AN X-RAY, OPTICAL AND INFRA-RED STUDY OF HIGH-MASS X-RAY BINARIES IN THE SMALL MAGELLANIC CLOUD by Lee John Townsend ...
White dwarf binary
... White dwarfs White dwarf limit White dwarf binary Accretion disks Thought question Nova Thought question 2 types of SN Nova or supernova? Standard candles Neutron stars Discovery Crab pulsar Pulsars Pulsars are NS! Magnetic fields Thought question Binaries Spin up Thought question ...
... White dwarfs White dwarf limit White dwarf binary Accretion disks Thought question Nova Thought question 2 types of SN Nova or supernova? Standard candles Neutron stars Discovery Crab pulsar Pulsars Pulsars are NS! Magnetic fields Thought question Binaries Spin up Thought question ...
A Variability Study of the Typical Red Supergiant Antares A
... with historical radial velocity measures, Hipparcos photometry, and AAVSO photometry. From these data we determine four scales of variability: ~7140 days, 2167 days, ~1260 days, and ~100 days. The longest of these periods is found from the AAVSO photometry and cannot be confirmed by any of the other ...
... with historical radial velocity measures, Hipparcos photometry, and AAVSO photometry. From these data we determine four scales of variability: ~7140 days, 2167 days, ~1260 days, and ~100 days. The longest of these periods is found from the AAVSO photometry and cannot be confirmed by any of the other ...
The Life Cycle of Stars: Supernovae in Starbursts by Jason Kezwer
... resolution is required in order to detect supernovae in the extremely bright nuclear environments of LIRGs. Alternatively, infrared spectroscopy would reveal the telltale spectral features of nuclear supernovae. Spectroscopic observations of the Arp 220 nuclei were conducted using Keck in July 2013 ...
... resolution is required in order to detect supernovae in the extremely bright nuclear environments of LIRGs. Alternatively, infrared spectroscopy would reveal the telltale spectral features of nuclear supernovae. Spectroscopic observations of the Arp 220 nuclei were conducted using Keck in July 2013 ...
Properties of White Dwarfs, Teacher Guide
... Some background: Sirius is a nearby star – only 9 light-years away. All stars in our Galaxy orbit the Galactic barycenter, so they are all moving. Astronomers detect and track the motion of stars relative to our Sun. There are two motions that can be measured: radial velocity (in the line of sight) ...
... Some background: Sirius is a nearby star – only 9 light-years away. All stars in our Galaxy orbit the Galactic barycenter, so they are all moving. Astronomers detect and track the motion of stars relative to our Sun. There are two motions that can be measured: radial velocity (in the line of sight) ...
A spectroscopic study of detached binary systems using precise radial velocities
... orbits, whilst others result from much more active processes, such as mass exchange leading to intense radiation emissions. A complete understanding of a binary system’s orbital characteristics, as well as the measurement of the all-important stellar masses, is almost always only achieved after the ...
... orbits, whilst others result from much more active processes, such as mass exchange leading to intense radiation emissions. A complete understanding of a binary system’s orbital characteristics, as well as the measurement of the all-important stellar masses, is almost always only achieved after the ...
Chandra Characterization of X-ray Emission in the Young F
... spectra than their lower mass brethren. For example, HD 100453 and the similarly aged 51 Eri (F0V) have coronal temperatures of about 0.2 keV as opposed to 1-2 keV for similarly aged GKM stars (Collins et al. 2009, Feigelson et al. 2006). Finally, the “FIP-effect” in which elements with first ioniza ...
... spectra than their lower mass brethren. For example, HD 100453 and the similarly aged 51 Eri (F0V) have coronal temperatures of about 0.2 keV as opposed to 1-2 keV for similarly aged GKM stars (Collins et al. 2009, Feigelson et al. 2006). Finally, the “FIP-effect” in which elements with first ioniza ...
Stellar Structure and Evolution
... given for several years to third-year undergraduate students in physics at the University of Aarhus. The goal of the course and the notes is to show how many aspects of stellar evolution can be understood relatively simply in terms of basic physics. Apart from the intrinsic interest of the topic, th ...
... given for several years to third-year undergraduate students in physics at the University of Aarhus. The goal of the course and the notes is to show how many aspects of stellar evolution can be understood relatively simply in terms of basic physics. Apart from the intrinsic interest of the topic, th ...
Structure in the first quadrant of the Galaxy: an analysis of TMGS star
... detailed analyses of the content of the IRAS sky (Walker et al. 1989). These comprise 33 ‘normal’ stellar types; 42 types of AGB star, both oxygen- and carbon-rich; six types of object that are distinct from others only in their MIR high luminosity; and six types of exotica including H ii regions, p ...
... detailed analyses of the content of the IRAS sky (Walker et al. 1989). These comprise 33 ‘normal’ stellar types; 42 types of AGB star, both oxygen- and carbon-rich; six types of object that are distinct from others only in their MIR high luminosity; and six types of exotica including H ii regions, p ...
Circumstellar dust emission from nearby Solar
... Far-infrared excess above the photosphere of a star indicates the presence of a circumstellar dust disc, which is a sign-post for extrasolar planets, and was first detected in the mid 1980s. Dust discs are intricately connected to planets and planetesimals, give insights in the dynamics and evolutio ...
... Far-infrared excess above the photosphere of a star indicates the presence of a circumstellar dust disc, which is a sign-post for extrasolar planets, and was first detected in the mid 1980s. Dust discs are intricately connected to planets and planetesimals, give insights in the dynamics and evolutio ...
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 masses and spins of neutron stars and stellar
... As the remnants of core-collapse supernovae, neutron stars and black holes are also windows into the collapse and explosion processes. The further evolution of these systems in accreting binaries can tell us about the accretion process, e.g., the total amount of mass that is typically deposited on t ...
... As the remnants of core-collapse supernovae, neutron stars and black holes are also windows into the collapse and explosion processes. The further evolution of these systems in accreting binaries can tell us about the accretion process, e.g., the total amount of mass that is typically deposited on t ...
Multiwavelength observations of XTE J1118+480`s outburst
... 30% of sources detected by INTEGRAL/IBIS were not known. 80% of Norma sources are X-ray pulsars, high spin periods Spectra typical of neutron stars No radio emission 85% of sources are highly absorbed (X-ray observations): column density NH>1023 cm-2 X-ray absorption >> IR => absorbing matter local ...
... 30% of sources detected by INTEGRAL/IBIS were not known. 80% of Norma sources are X-ray pulsars, high spin periods Spectra typical of neutron stars No radio emission 85% of sources are highly absorbed (X-ray observations): column density NH>1023 cm-2 X-ray absorption >> IR => absorbing matter local ...
Annual Report 2006/2007
... The ultimate goal of astronomical research is to understand the Universe and the objects within it in terms of the laws of physics. Questions concerning the nature and evolution of the Universe are profound and appeal to a deep human desire to understand our place in the Universe. They relate direct ...
... The ultimate goal of astronomical research is to understand the Universe and the objects within it in terms of the laws of physics. Questions concerning the nature and evolution of the Universe are profound and appeal to a deep human desire to understand our place in the Universe. They relate direct ...
Stars: HR Diagaram Stellar Evolution Astronomy 1 — Elementary Astronomy LA Mission College
... LA Mission College Spring F2015 ...
... LA Mission College Spring F2015 ...
Axisymmetry in protoplanetary nebulae: using imaging polarimetry
... any further outflow along the polar axis. Until recently, however, resolved images of CSEs existed for only a few large, bipolar PPNe, compared with a list of PPNe candidates numbering over 100 (Volk & Kwok 1989), and so this model has not been well tested. In many PPNe, the dust shell has thinned t ...
... any further outflow along the polar axis. Until recently, however, resolved images of CSEs existed for only a few large, bipolar PPNe, compared with a list of PPNe candidates numbering over 100 (Volk & Kwok 1989), and so this model has not been well tested. In many PPNe, the dust shell has thinned t ...
Understanding Variable Stars - Central Florida Astronomical Society
... perspective, an introduction to stars in general, the techniques for discovering and studying variable stars, and a description of the main types of variable stars. It ends with short reflections about the connection between the study of variable stars, and research, education, amateur astronomy, and ...
... perspective, an introduction to stars in general, the techniques for discovering and studying variable stars, and a description of the main types of variable stars. It ends with short reflections about the connection between the study of variable stars, and research, education, amateur astronomy, and ...
Astronomy Astrophysics - Niels Bohr Institutet
... also recalibrated and redetermined the astrophysical parameters (T eff , Mv , and [Fe/H]) for all stars in our sample. Much effort has been devoted to the fundamental issue of determining reliable isochrone ages for as many stars as possible, and we believe that a rather more realistic assessment of t ...
... also recalibrated and redetermined the astrophysical parameters (T eff , Mv , and [Fe/H]) for all stars in our sample. Much effort has been devoted to the fundamental issue of determining reliable isochrone ages for as many stars as possible, and we believe that a rather more realistic assessment of t ...
Radio pulsars
... • Young pulsars have unpredictable changes in period glitches and period noise. • Millisecond pulsars have extremely stable periods. ...
... • Young pulsars have unpredictable changes in period glitches and period noise. • Millisecond pulsars have extremely stable periods. ...
Lyra
Lyra (/ˈlaɪərə/; Latin for lyre, from Greek λύρα) is a small constellation. It is one of 48 listed by the 2nd century astronomer Ptolemy, and is one of the 88 constellations recognized by the International Astronomical Union. Lyra was often represented on star maps as a vulture or an eagle carrying a lyre, and hence sometimes referred to as Aquila Cadens or Vultur Cadens. Beginning at the north, Lyra is bordered by Draco, Hercules, Vulpecula, and Cygnus. Lyra is visible from the northern hemisphere from spring through autumn, and nearly overhead, in temperate latitudes, during the summer months. From the southern hemisphere, it is visible low in the northern sky during the winter months.The lucida or brightest star—and one of the brightest stars in the sky—is the white main sequence star Vega, a corner of the Summer Triangle. Beta Lyrae is the prototype of a class of stars known as Beta Lyrae variables, binary stars so close to each other that they become egg-shaped and material flows from one to the other. Epsilon Lyrae, known informally as the Double Double, is a complex multiple star system. Lyra also hosts the Ring Nebula, the second-discovered and best-known planetary nebula.