Glossary Topics - Home - DMNS Galaxy Guide Portal
... the star to heat and cool, expand and contract. The very most massive stars are so luminous they blow off their outer layers. The remaining star, called a Wolf-Rayet star, is recognizable by its strange spectrum. Once the material at the core is burned to iron, the star faces the ultimate energy cri ...
... the star to heat and cool, expand and contract. The very most massive stars are so luminous they blow off their outer layers. The remaining star, called a Wolf-Rayet star, is recognizable by its strange spectrum. Once the material at the core is burned to iron, the star faces the ultimate energy cri ...
Astronomy 111 – Lecture 2
... – There is a time when it is light. = Day – There is a time when it is dark. = Night ...
... – There is a time when it is light. = Day – There is a time when it is dark. = Night ...
Mysteries of Space
... • Form from the death of a very large star ( more than 25 solar masses). A supernova occurs followed by a black hole • Strangest objects in the universe • Their existence was predicted before they were discovered • When astronomers say they have found a black hole, they have not seen it but have det ...
... • Form from the death of a very large star ( more than 25 solar masses). A supernova occurs followed by a black hole • Strangest objects in the universe • Their existence was predicted before they were discovered • When astronomers say they have found a black hole, they have not seen it but have det ...
Stellar Spectra Classification
... Introduction: Classifying stars based on brightness is somewhat problematic. A star’s apparent brightness can be affected by its distance from the observer, its size, or by the presence of interstellar dust. Instead, astronomers classify stars based on the major components of their spectra. Much lik ...
... Introduction: Classifying stars based on brightness is somewhat problematic. A star’s apparent brightness can be affected by its distance from the observer, its size, or by the presence of interstellar dust. Instead, astronomers classify stars based on the major components of their spectra. Much lik ...
m 1
... 1. Use stars < 100pc to calibrate MV for spectral classes 2. For unknown star: a) use CCD to measure mV b) use spectrograph to find spectral class c) use calibration from (1) to get MV d) use distance modulus to calculate d ...
... 1. Use stars < 100pc to calibrate MV for spectral classes 2. For unknown star: a) use CCD to measure mV b) use spectrograph to find spectral class c) use calibration from (1) to get MV d) use distance modulus to calculate d ...
The origin of magnetism on the upper main sequence
... disc fragmentation, competitive accretion and close dynamical interactions all playing a role. Current ideas have been developed to take account of the observations that stars form in highly turbulent, high-density regions, that they form in relatively dense clusters and that most of them are in bin ...
... disc fragmentation, competitive accretion and close dynamical interactions all playing a role. Current ideas have been developed to take account of the observations that stars form in highly turbulent, high-density regions, that they form in relatively dense clusters and that most of them are in bin ...
UNIVERSITY OF BRISTOL
... What is meant by a de Vaucouleurs (or r1/4) profile and for which galaxy type is it appropriate? How does the Sersic profile differ from this? (b) (12 marks) The bulge and disc components of a certain galaxy are observed to have half light (effective) radii of 3 arcsec and 15 arcsec, and surface bri ...
... What is meant by a de Vaucouleurs (or r1/4) profile and for which galaxy type is it appropriate? How does the Sersic profile differ from this? (b) (12 marks) The bulge and disc components of a certain galaxy are observed to have half light (effective) radii of 3 arcsec and 15 arcsec, and surface bri ...
DM in the Galaxy - University of Oxford
... Near Sun data consistent with expected DM halo At R ¿ R0 non-circular motions constrain contribution of axisymmetric component; microlensing ¿ only slightly overpredicted when all matter stellar, but probably room for cosmologically favoured dark halo ...
... Near Sun data consistent with expected DM halo At R ¿ R0 non-circular motions constrain contribution of axisymmetric component; microlensing ¿ only slightly overpredicted when all matter stellar, but probably room for cosmologically favoured dark halo ...
SN 2004dj
... SN in M51! (SN 2005cs) Stellar explosion with giant energy release Energy of the visible explosion~1051 ergs Luminosity~109-10 L⊙ Supernovae might be the brightest objects in the universe, and can outshine a whole galaxy (for a few weeks) ...
... SN in M51! (SN 2005cs) Stellar explosion with giant energy release Energy of the visible explosion~1051 ergs Luminosity~109-10 L⊙ Supernovae might be the brightest objects in the universe, and can outshine a whole galaxy (for a few weeks) ...
n - Ira-Inaf
... Mg, Al, Na, K, Ca, Ti underabundant wrt the solar composition as atoms & molecules (cold) ions +electrons (hot) average number density = 1 cm3 quantum processes then line emission/a ...
... Mg, Al, Na, K, Ca, Ti underabundant wrt the solar composition as atoms & molecules (cold) ions +electrons (hot) average number density = 1 cm3 quantum processes then line emission/a ...
TRANSIT
... groups - together with other young people – on astronomical projects. The projects vary from night-time observations to theoretical problems, depending on your own interests. The working groups will be led by young scientists from the IAYC team. The IAYC 2009 will offer a wide range of working grou ...
... groups - together with other young people – on astronomical projects. The projects vary from night-time observations to theoretical problems, depending on your own interests. The working groups will be led by young scientists from the IAYC team. The IAYC 2009 will offer a wide range of working grou ...
Your Place in Space and Time
... The background illustration depicts the overall distribution of galaxies in our observable universe; individual galaxies are microscopic on this scale. The portion of the universe that we can observe is limited by the age of the universe: Because our universe is about 14 billion years old, we can se ...
... The background illustration depicts the overall distribution of galaxies in our observable universe; individual galaxies are microscopic on this scale. The portion of the universe that we can observe is limited by the age of the universe: Because our universe is about 14 billion years old, we can se ...
PowerPoint version is here
... How it works! Gravity pushes inward, but the center of the sun in heated by nuclear reactions, making a high pressure that pushes outwards. They balance, and the sun just sits there burning its nuclear fuel. This has gone on for 4.5 billion years and will continue for another 5 billion years. ...
... How it works! Gravity pushes inward, but the center of the sun in heated by nuclear reactions, making a high pressure that pushes outwards. They balance, and the sun just sits there burning its nuclear fuel. This has gone on for 4.5 billion years and will continue for another 5 billion years. ...
Module Outlines
... magnitude 1 – the brightest stars magnitude 2 magnitude 3 magnitude 4 magnitude 5 magnitude 6 – the faintest stars Today, the magnitude system has been extended to include much fainter and brighter objects. ...
... magnitude 1 – the brightest stars magnitude 2 magnitude 3 magnitude 4 magnitude 5 magnitude 6 – the faintest stars Today, the magnitude system has been extended to include much fainter and brighter objects. ...
Star Track 2 - The Search for a Supermassive Black... Early radio astronomers detected an immensely
... - There is no detectable optical or infrared emission from this source. We don't know of any practical way for millions of solar masses of material to not radiate optically fainter than an ordinary star other than a black hole. - There is, however, powerful radio emission coming from the source, exp ...
... - There is no detectable optical or infrared emission from this source. We don't know of any practical way for millions of solar masses of material to not radiate optically fainter than an ordinary star other than a black hole. - There is, however, powerful radio emission coming from the source, exp ...
Midterm Study Game
... Which two Earth spheres are interacting if a lightning strike were to start a forest fire? A. Atmosphere and biosphere B. Biosphere and hydrosphere C. Atmosphere and geosphere D. Hydrosphere and biosphere Next up 1s ...
... Which two Earth spheres are interacting if a lightning strike were to start a forest fire? A. Atmosphere and biosphere B. Biosphere and hydrosphere C. Atmosphere and geosphere D. Hydrosphere and biosphere Next up 1s ...
Methods of Determining Relative Age of Young Stellar Objects
... rapidly fluctuate with temperature, spectral type, wind outflows and inflows and magnitude. Some also have spectral anomalies which may indicate the presence of circum-stellar dust. Spectral types of these stars range from B type to K and they have irregular periods, varying by up to four magnitudes ...
... rapidly fluctuate with temperature, spectral type, wind outflows and inflows and magnitude. Some also have spectral anomalies which may indicate the presence of circum-stellar dust. Spectral types of these stars range from B type to K and they have irregular periods, varying by up to four magnitudes ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.