3-color photometry of stellar cluster - Kiepenheuer
... and from the sky are more severe near horizon. Due to the wavelenght dependant scattering cross-section, blue is affected the most followed by green and red (Weigert and Wendker, 1989). Lastly the observatory at Schauinsland is surrounded thees by which helps with straylight from the cities but rest ...
... and from the sky are more severe near horizon. Due to the wavelenght dependant scattering cross-section, blue is affected the most followed by green and red (Weigert and Wendker, 1989). Lastly the observatory at Schauinsland is surrounded thees by which helps with straylight from the cities but rest ...
All_Stars
... When the core fuel source is exhausted in massive stars, they contract and heat up to temperatures sufficient to ignite fusion in the “ash” left over from the previous core-burning stage. The final burning stage is silicon (Si) to iron (Fe) in the core. Fusion of lighter elements occurs in shells su ...
... When the core fuel source is exhausted in massive stars, they contract and heat up to temperatures sufficient to ignite fusion in the “ash” left over from the previous core-burning stage. The final burning stage is silicon (Si) to iron (Fe) in the core. Fusion of lighter elements occurs in shells su ...
Star Stuff
... - divides the light up into its colors (wavelengths) - use a smaller range of wavelengths than entire EM spectrum because instrumentation is different ...
... - divides the light up into its colors (wavelengths) - use a smaller range of wavelengths than entire EM spectrum because instrumentation is different ...
SPECTRAL ANALYSIS OF A NEWLY DISCOVERED HgMn STAR
... 4500-5840 Å. The data were obtained with the multi-fiber spectrograph GIRAFFE with MEDUSA, mounted at UT2 (Kueyen), the 8 meter class VLT telescope, in Chile. The atmospheric parameters of the star were determined from Geneva photometry and hydrogen line modeling (Te = 12000 ± 200 K, log g = 4.1 ± ü ...
... 4500-5840 Å. The data were obtained with the multi-fiber spectrograph GIRAFFE with MEDUSA, mounted at UT2 (Kueyen), the 8 meter class VLT telescope, in Chile. The atmospheric parameters of the star were determined from Geneva photometry and hydrogen line modeling (Te = 12000 ± 200 K, log g = 4.1 ± ü ...
Astrophysics
... • Hubble found (using Cepheids) that certain 'nebulae' were not dust clouds, as had been thought, but distant galaxies. He used Cepheid variables in the nebulae to show that they were much further away than any stars in the Milky Way. (Cepheids are bright stars with a predictable luminosity-period r ...
... • Hubble found (using Cepheids) that certain 'nebulae' were not dust clouds, as had been thought, but distant galaxies. He used Cepheid variables in the nebulae to show that they were much further away than any stars in the Milky Way. (Cepheids are bright stars with a predictable luminosity-period r ...
Lecture (Powerpoint)
... Any particularly dense regions can (for a while) protect columns in their shadow ...
... Any particularly dense regions can (for a while) protect columns in their shadow ...
plagiarism - Homeschool
... How to use the info without plagiarizing: surface would reach all the way out to Everything has a temperature, and Jupiter. Betelgeuse's color is bright red. everything radiates light, and the two are On the other hand, another supergiant not unconnected. In fact, the hotter a body star, Rigel, with ...
... How to use the info without plagiarizing: surface would reach all the way out to Everything has a temperature, and Jupiter. Betelgeuse's color is bright red. everything radiates light, and the two are On the other hand, another supergiant not unconnected. In fact, the hotter a body star, Rigel, with ...
File
... fusion is a process in which less-massive atomic nuclei combine to form more-massive nuclei. The process releases enormous amounts of energy. • The onset of nuclear fusion marks the birth of a star. Once this process begins, it can continue for billions of years. ...
... fusion is a process in which less-massive atomic nuclei combine to form more-massive nuclei. The process releases enormous amounts of energy. • The onset of nuclear fusion marks the birth of a star. Once this process begins, it can continue for billions of years. ...
Multiple Choice, continued
... fusion is a process in which less-massive atomic nuclei combine to form more-massive nuclei. The process releases enormous amounts of energy. • The onset of nuclear fusion marks the birth of a star. Once this process begins, it can continue for billions of years. ...
... fusion is a process in which less-massive atomic nuclei combine to form more-massive nuclei. The process releases enormous amounts of energy. • The onset of nuclear fusion marks the birth of a star. Once this process begins, it can continue for billions of years. ...
1. Introduction
... In parallel with these developments, it has come to be realized that some, and probably very many, stars pulsate in more complicated manners than the Cepheids. In many instances more than one mode of oscillation is excited simultaneously in a star; these modes may include both radial overtones, in a ...
... In parallel with these developments, it has come to be realized that some, and probably very many, stars pulsate in more complicated manners than the Cepheids. In many instances more than one mode of oscillation is excited simultaneously in a star; these modes may include both radial overtones, in a ...
Stars, Galaxies, and the Universe Section 1 Section 1
... • The apparent motion of stars, or motion as it appears from Earth, is caused by the movement of Earth. • The stars seem as though they are moving counterclockwise around a central star called Polaris, the North Star. Polaris is almost directly above the North Pole, and thus the star does not appear ...
... • The apparent motion of stars, or motion as it appears from Earth, is caused by the movement of Earth. • The stars seem as though they are moving counterclockwise around a central star called Polaris, the North Star. Polaris is almost directly above the North Pole, and thus the star does not appear ...
Aries The Ram - Maverick`s E-portfolio
... discovered inside the galaxy. NGC 772 is just less than 130 light years away from earth and has a apparent magnitude of 11.3. NGC 772 is a satellite galaxy and neighbors with a elliptical galaxy named NGC 770. This galaxy has an apparent magnitude of 14.2[5]. Aries is most known to astronomers for i ...
... discovered inside the galaxy. NGC 772 is just less than 130 light years away from earth and has a apparent magnitude of 11.3. NGC 772 is a satellite galaxy and neighbors with a elliptical galaxy named NGC 770. This galaxy has an apparent magnitude of 14.2[5]. Aries is most known to astronomers for i ...
ph507lecnote06
... Most stars have properties within the shaded region known as the main sequence. The points plotted here are for stars lying within about 5 pc of the Sun. The diagonal lines correspond to constant stellar radius, so that stellar size can be represented on the same diagram as luminosity and temperatur ...
... Most stars have properties within the shaded region known as the main sequence. The points plotted here are for stars lying within about 5 pc of the Sun. The diagonal lines correspond to constant stellar radius, so that stellar size can be represented on the same diagram as luminosity and temperatur ...
Project 4: The HR diagram. Open clusters
... Exercise 2: Sirius is about twice as massive as the Sun. How much brighter is it with respect to the Sun? In the HR diagram, where will you find the least massive stars? and the most massive stars? If I double the mass of a main sequence star, the luminosity increases by a factor 2 3.5 ~ 11.3. ...
... Exercise 2: Sirius is about twice as massive as the Sun. How much brighter is it with respect to the Sun? In the HR diagram, where will you find the least massive stars? and the most massive stars? If I double the mass of a main sequence star, the luminosity increases by a factor 2 3.5 ~ 11.3. ...
Celestial Distances
... Summary (cont’d) For distant stars that are not variable and don’t have a nearby variable star, use the temperature - luminosity relation of the H-R diagram. Does require some work to determine if the star is main sequence, dwarf, or giant. Later we will see the use of red shift and supernovae ...
... Summary (cont’d) For distant stars that are not variable and don’t have a nearby variable star, use the temperature - luminosity relation of the H-R diagram. Does require some work to determine if the star is main sequence, dwarf, or giant. Later we will see the use of red shift and supernovae ...
CONSTELLATIONS
... • Since the Earth is rotating constantly, the Right Ascension "value" changes continuously - every minute of the night. It also changes every day of the year as Earth goes around the Sun. We start this numbering system at the Vernal Equinox i.e. the point in the sky where the Sun was at the time of ...
... • Since the Earth is rotating constantly, the Right Ascension "value" changes continuously - every minute of the night. It also changes every day of the year as Earth goes around the Sun. We start this numbering system at the Vernal Equinox i.e. the point in the sky where the Sun was at the time of ...
Solutions
... (c) All you can really conclude is: although average stars have much more of the Galaxy’s mass than luminous main sequence stars, those luminous main sequence stars put out more light than all those average stars put together. Note: A few of you made the equation “more mass equals more luminosity”. ...
... (c) All you can really conclude is: although average stars have much more of the Galaxy’s mass than luminous main sequence stars, those luminous main sequence stars put out more light than all those average stars put together. Note: A few of you made the equation “more mass equals more luminosity”. ...
Stellar Evolution: the Death of Stars
... – Type 1a supernova: explosion of white dwarf in a closed binary system; mass accumulation exceeds the critical mass and ignites the carbon fusion at the core – Type 1b supernova: core collapse of massive star with hydrogen shell lost before – Type 1c supernova: core collapse of massive star with bo ...
... – Type 1a supernova: explosion of white dwarf in a closed binary system; mass accumulation exceeds the critical mass and ignites the carbon fusion at the core – Type 1b supernova: core collapse of massive star with hydrogen shell lost before – Type 1c supernova: core collapse of massive star with bo ...
Lecture 13 - Star Formation
... A star has 4 times the mass and 128 times the luminosity of the Sun. The star's lifetime will be ____ times that of Sun. A) 32 B) 4 C) 1 D) ¼ E) 1/32 ...
... A star has 4 times the mass and 128 times the luminosity of the Sun. The star's lifetime will be ____ times that of Sun. A) 32 B) 4 C) 1 D) ¼ E) 1/32 ...
Pallavicini - IASF Milano
... Cluster age about 50 Myr, d=190 pc 275 ks combined exp time, 154 X-ray sources detected with ML > 10: only 13 cluster members in the XMM field, all but one detected (sensitivity at field center : 7x1027 erg/s, an order of magnitude higher than the previous ROSAT observations). ...
... Cluster age about 50 Myr, d=190 pc 275 ks combined exp time, 154 X-ray sources detected with ML > 10: only 13 cluster members in the XMM field, all but one detected (sensitivity at field center : 7x1027 erg/s, an order of magnitude higher than the previous ROSAT observations). ...
Corona Australis
Corona Australis /kɵˈroʊnə ɒˈstreɪlɨs/ or Corona Austrina /kɵˈroʊnə ɒˈstraɪnə/ is a constellation in the Southern Celestial Hemisphere. Its Latin name means ""southern crown"", and it is the southern counterpart of Corona Borealis, the northern crown. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations. The Ancient Greeks saw Corona Australis as a wreath rather than a crown and associated it with Sagittarius or Centaurus. Other cultures have likened the pattern to a turtle, ostrich nest, a tent, or even a hut belonging to a rock hyrax.Although fainter than its namesake, the oval- or horseshoe-shaped pattern of its brighter stars renders it distinctive. Alpha and Beta Coronae Australis are the two brightest stars with an apparent magnitude of around 4.1. Epsilon Coronae Australis is the brightest example of a W Ursae Majoris variable in the southern sky. Lying alongside the Milky Way, Corona Australis contains one of the closest star-forming regions to our Solar System—a dusty dark nebula known as the Corona Australis Molecular Cloud, lying about 430 light years away. Within it are stars at the earliest stages of their lifespan. The variable stars R and TY Coronae Australis light up parts of the nebula, which varies in brightness accordingly.