Astronomical Distance Determination
... Our eyes have evolved to be most sensitive to the light emitted by the sun. Hence the bolometric correction for the missed emission in the infrared and ultraviolet is small for the sun. The “visual” magnitude actually corresponds to the flux measured with a certain filter on the telescope. There are ...
... Our eyes have evolved to be most sensitive to the light emitted by the sun. Hence the bolometric correction for the missed emission in the infrared and ultraviolet is small for the sun. The “visual” magnitude actually corresponds to the flux measured with a certain filter on the telescope. There are ...
Metallicity maps
... Ram-pressure stripping can produce considerably more metals than galactic winds (depending on cluster mass and other cluster properties) Schindler et al. 2005, Kapferer et al. 2007, 2009 ...
... Ram-pressure stripping can produce considerably more metals than galactic winds (depending on cluster mass and other cluster properties) Schindler et al. 2005, Kapferer et al. 2007, 2009 ...
Studying Variable stars using Small Telescopes Observational
... RS CVn binaries Brightness variation is due to the spots (similar to sunspots) on the surface of stars. As a star with spots rotates, its brightness changes. ...
... RS CVn binaries Brightness variation is due to the spots (similar to sunspots) on the surface of stars. As a star with spots rotates, its brightness changes. ...
Radiatively driven Rayleigh-Taylor instability candidates around a
... young, and extraordinarily luminous. Massive (OB-type) stars are very few, representing just over 0.1% of all main-sequence stars in our Galaxy. Thus, stringent conditions on observations and target selection exist in order to verify the validity of theoretical scenarios. The UCHII region G333.6-0.2 ...
... young, and extraordinarily luminous. Massive (OB-type) stars are very few, representing just over 0.1% of all main-sequence stars in our Galaxy. Thus, stringent conditions on observations and target selection exist in order to verify the validity of theoretical scenarios. The UCHII region G333.6-0.2 ...
Star-S_Teacher_Guide - The University of Texas at Dallas
... problem is that fire, a chemical reaction, does not produce much energy in comparison with fusion. Before this century, the accepted view was that the Sun, and therefore the stars, shines because of a chemical process such as fire. If the Sun were a coal furnace, an idea from the last century, then ...
... problem is that fire, a chemical reaction, does not produce much energy in comparison with fusion. Before this century, the accepted view was that the Sun, and therefore the stars, shines because of a chemical process such as fire. If the Sun were a coal furnace, an idea from the last century, then ...
The Evening Sky Map
... Conjunction – An alignment of two celestial bodies such that they present the least angular separation as viewed from Earth. Constellation – A defined area of the sky containing a star pattern. Diffuse Nebula – A cloud of gas illuminated by nearby stars. Double Star – Two stars that appear close to ...
... Conjunction – An alignment of two celestial bodies such that they present the least angular separation as viewed from Earth. Constellation – A defined area of the sky containing a star pattern. Diffuse Nebula – A cloud of gas illuminated by nearby stars. Double Star – Two stars that appear close to ...
Question Paper - SAVE MY EXAMS!
... 13 The interior of a star has conditions that are ideal for sustainable fusion reactions. The general conditions for fusion require a very large A amount of hydrogen and temperature. B amount of hydrogen and pressure. C density and pressure. D density and temperature. (Total for Question = 1 mark) 1 ...
... 13 The interior of a star has conditions that are ideal for sustainable fusion reactions. The general conditions for fusion require a very large A amount of hydrogen and temperature. B amount of hydrogen and pressure. C density and pressure. D density and temperature. (Total for Question = 1 mark) 1 ...
REACH FOR THE STARS MLK 2009
... 7. What was Messier looking for when he made his observations? _________________ 8. Why are there so few M Objects in the southern skies? __________________________________ 9. When did M 1 SN? _____________________ 10. What do Cas A and Tycho in Cassiopeia have in common? ___________________________ ...
... 7. What was Messier looking for when he made his observations? _________________ 8. Why are there so few M Objects in the southern skies? __________________________________ 9. When did M 1 SN? _____________________ 10. What do Cas A and Tycho in Cassiopeia have in common? ___________________________ ...
a report on pulsars, written for PHAS1901
... telescope (and many cannot be seen anyway), so absolute magnitudes cannot be used to determine their distances from us; other methods must be employed, such as measurment of dispersion. All electromagnetic radiation moves at a constant speed through a vacuum, but is slowed proportionally to it's wav ...
... telescope (and many cannot be seen anyway), so absolute magnitudes cannot be used to determine their distances from us; other methods must be employed, such as measurment of dispersion. All electromagnetic radiation moves at a constant speed through a vacuum, but is slowed proportionally to it's wav ...
Properties of Stars - Indiana State University
... ionized state • A stars have just the right temperature to put electrons into hydrogen’s 2nd energy level, which results in strong absorption lines in the visible • F, G, and K stars are of a low enough temperature to show absorption lines of metals such as calcium and iron, elements that are typica ...
... ionized state • A stars have just the right temperature to put electrons into hydrogen’s 2nd energy level, which results in strong absorption lines in the visible • F, G, and K stars are of a low enough temperature to show absorption lines of metals such as calcium and iron, elements that are typica ...
Robert_Minchin_Galaxies_2011_REU
... clusters have similar morphologies and similar luminosities. • How do we decide what is a globular cluster and what is a galaxy? • Dynamics! ...
... clusters have similar morphologies and similar luminosities. • How do we decide what is a globular cluster and what is a galaxy? • Dynamics! ...
L101 DETECTION OF A LARGE ARC OF IONIZED HYDROGEN
... A close relationship between this Ha loop and the W4 chimney is suggested by both appearance and kinematics. Unfortunately, at Galactic latitudes below about 10⬚, the surface brightness of the large loop is less than that of the more diffuse ionized gas in the Perseus arm and can no longer be identi ...
... A close relationship between this Ha loop and the W4 chimney is suggested by both appearance and kinematics. Unfortunately, at Galactic latitudes below about 10⬚, the surface brightness of the large loop is less than that of the more diffuse ionized gas in the Perseus arm and can no longer be identi ...
Scientific requirements of ALMA, and its capabilities for key
... Image gas kinematics in protostars and protoplanetary disks around Sun-like stars at 140pc distance, enabling one to study their physical, chemical and magnetic field structures and to detect the gaps created by planets undergoing formation in the disk. Provide precise images at 0.1 arcsec resolutio ...
... Image gas kinematics in protostars and protoplanetary disks around Sun-like stars at 140pc distance, enabling one to study their physical, chemical and magnetic field structures and to detect the gaps created by planets undergoing formation in the disk. Provide precise images at 0.1 arcsec resolutio ...
Supplementary Information
... colour but is otherwise close to the median values of the full sample in terms of its stellar mass and star formation rate (Fig.S1). In contrast, optically-selected star-forming z~2 galaxies, in particular BM/BX objects, typically are fainter in the K-band, have lower stellar masses (median ~2x1010 ...
... colour but is otherwise close to the median values of the full sample in terms of its stellar mass and star formation rate (Fig.S1). In contrast, optically-selected star-forming z~2 galaxies, in particular BM/BX objects, typically are fainter in the K-band, have lower stellar masses (median ~2x1010 ...
X-ray Emission from Massive Stars
... *don’t forget that thermal emitters give off photons with a range of wavelengths; those listed above represent the peak of the distribution or the characteristic wavelength. ...
... *don’t forget that thermal emitters give off photons with a range of wavelengths; those listed above represent the peak of the distribution or the characteristic wavelength. ...
Rearrangement of gas in disc galaxies
... Among most interesting physical phenomena in modern astrophysics are intense and sudden bursts of star formation and non-thermal activity in centres of galaxies. It is commonly accepted that starbursts are enhancements of star formation and the nuclear activity is generated by accretion of matter on ...
... Among most interesting physical phenomena in modern astrophysics are intense and sudden bursts of star formation and non-thermal activity in centres of galaxies. It is commonly accepted that starbursts are enhancements of star formation and the nuclear activity is generated by accretion of matter on ...
Project 4: The HR diagram. Open clusters
... of a star. From the figure, one sees that most stars fall along a diagonal strip from high temperature, high luminosity stars to low temperature, low luminosity stars. These are the main sequence stars. Our Sun is one of them. There are a few stars that are not in this diagonal strip. ...
... of a star. From the figure, one sees that most stars fall along a diagonal strip from high temperature, high luminosity stars to low temperature, low luminosity stars. These are the main sequence stars. Our Sun is one of them. There are a few stars that are not in this diagonal strip. ...
- IRSF: Past and Future
... Study of the gamma-ray binaries via near-infrared photometric monitoring Yuki Moritani (Univ Tokyo/Kavli IPMU) Gamma-ray binaries are a subclass of X-ray binaries that emit the majority of the energy in the gamma-ray band. They are comprised of a compact object and a massive (>10 Msun) star with a c ...
... Study of the gamma-ray binaries via near-infrared photometric monitoring Yuki Moritani (Univ Tokyo/Kavli IPMU) Gamma-ray binaries are a subclass of X-ray binaries that emit the majority of the energy in the gamma-ray band. They are comprised of a compact object and a massive (>10 Msun) star with a c ...
Pulsating variable stars and the Hertzsprung
... stars in different stages of their evolution. It is a plot showing a relationship between luminosity (or absolute magnitude) and stars' surface temperature (or spectral type). The bottom scale is ranging from high-temperature blue-white stars (left side of the diagram) to low-temperature red stars ( ...
... stars in different stages of their evolution. It is a plot showing a relationship between luminosity (or absolute magnitude) and stars' surface temperature (or spectral type). The bottom scale is ranging from high-temperature blue-white stars (left side of the diagram) to low-temperature red stars ( ...
star a
... Photometry and Color Ratios: Photometry measures the apparent brightness of a star. The color ratios of a star are the ratios of brightness values obtained through different standard filters, such as the U, B, and V filters. These ratios are a measure of the star’s surface temperature. Spectral Type ...
... Photometry and Color Ratios: Photometry measures the apparent brightness of a star. The color ratios of a star are the ratios of brightness values obtained through different standard filters, such as the U, B, and V filters. These ratios are a measure of the star’s surface temperature. Spectral Type ...
Astrophysics Questions (DRAFT)
... 94. Sketch a typical cooling function (T ) for di use interstellar gas and identify its prominent features. Overplot a hypothetical heating curve and show how to identify points of thermal equilibrium and their stability. 95. Explain the physics of 21 cm radio emission from neutral hydrogen atoms. ...
... 94. Sketch a typical cooling function (T ) for di use interstellar gas and identify its prominent features. Overplot a hypothetical heating curve and show how to identify points of thermal equilibrium and their stability. 95. Explain the physics of 21 cm radio emission from neutral hydrogen atoms. ...
two dozen compact sources and a massive disk
... theoretical papers in 1970s: – First appearance in a paper abstract: M. Disney (1975), “Boundary and Initial Conditions in Protostar Calculations” – First appearance in a paper title: Ferraioli & Virgopia (1979), “On the Mass Distribution Law of Systems of Protocluster Fragments” • Observational pap ...
... theoretical papers in 1970s: – First appearance in a paper abstract: M. Disney (1975), “Boundary and Initial Conditions in Protostar Calculations” – First appearance in a paper title: Ferraioli & Virgopia (1979), “On the Mass Distribution Law of Systems of Protocluster Fragments” • Observational pap ...
Notes (PowerPoint)
... • Some people say that science is just another set of beliefs • Scientists base their claims to truth on sensory evidence – experiments (direct experience) • Some religious people say the senses are not reliable; that faith wins out over (trumps) the five senses o Most religions accept science, in i ...
... • Some people say that science is just another set of beliefs • Scientists base their claims to truth on sensory evidence – experiments (direct experience) • Some religious people say the senses are not reliable; that faith wins out over (trumps) the five senses o Most religions accept science, in i ...
The Teleological Argument - University of Colorado Boulder
... if smaller: gravitational tug-of-wars would destabilize the sun's orbit 15. density of galaxy cluster if denser: galaxy collisions and mergers would disrupt the sun's orbit if less dense: star formation late enough in the history of the universe would be hampered by lack of material 16. average dist ...
... if smaller: gravitational tug-of-wars would destabilize the sun's orbit 15. density of galaxy cluster if denser: galaxy collisions and mergers would disrupt the sun's orbit if less dense: star formation late enough in the history of the universe would be hampered by lack of material 16. average dist ...
The mass function of star clusters formed in turbulent molecular clouds
... In the MW: The most massive GMC =~107Msun -> The most massive cluster = ~104Msun -> The most massive star = ~150Msun ...
... In the MW: The most massive GMC =~107Msun -> The most massive cluster = ~104Msun -> The most massive star = ~150Msun ...
H II region
An H II region is a large, low-density cloud of partially ionized gas in which star formation has recently taken place. The short-lived blue stars forged in these regions emit copious amounts of ultraviolet light that ionize the surrounding gas. H II regions—sometimes several hundred light-years across—are often associated with giant molecular clouds. The first known H II region was the Orion Nebula, which was discovered in 1610 by Nicolas-Claude Fabri de Peiresc.H II regions are named for the large amount of ionised atomic hydrogen they contain, referred to as H II, pronounced H-two by astronomers (an H I region being neutral atomic hydrogen, and H2 being molecular hydrogen). Such regions have extremely diverse shapes, because the distribution of the stars and gas inside them is irregular. They often appear clumpy and filamentary, sometimes showing bizarre shapes such as the Horsehead Nebula. H II regions may give birth to thousands of stars over a period of several million years. In the end, supernova explosions and strong stellar winds from the most massive stars in the resulting star cluster will disperse the gases of the H II region, leaving behind a cluster of birthed stars such as the Pleiades.H II regions can be seen to considerable distances in the universe, and the study of extragalactic H II regions is important in determining the distance and chemical composition of other galaxies. Spiral and irregular galaxies contain many H II regions, while elliptical galaxies are almost devoid of them. In the spiral galaxies, including the Milky Way, H II regions are concentrated in the spiral arms, while in the irregular galaxies they are distributed chaotically. Some galaxies contain huge H II regions, which may contain tens of thousands of stars. Examples include the 30 Doradus region in the Large Magellanic Cloud and NGC 604 in the Triangulum Galaxy.