ASTR 1101-001 Spring 2008 - Louisiana State University
... sunrise, a new and dazzling object ascended above the eastern horizon. This “guest star” was so brilliant that it could easily be seen during broad daylight for the rest of July! This “guest star” was visible in the night sky (to the naked eye) for 21 months. ...
... sunrise, a new and dazzling object ascended above the eastern horizon. This “guest star” was so brilliant that it could easily be seen during broad daylight for the rest of July! This “guest star” was visible in the night sky (to the naked eye) for 21 months. ...
1_Introduction
... The radial velocity of a star is found from its Doppler shift. Radial velocity = how fast an object is moving toward you or away from you. ...
... The radial velocity of a star is found from its Doppler shift. Radial velocity = how fast an object is moving toward you or away from you. ...
File
... star’s properties? • Star radii differ greatly – Most are roughly the size of our Sun – Some, like Betelgeuse, are hundreds of times larger. These are Giants – Smaller stars, including our Sun, are Dwarfs, or ...
... star’s properties? • Star radii differ greatly – Most are roughly the size of our Sun – Some, like Betelgeuse, are hundreds of times larger. These are Giants – Smaller stars, including our Sun, are Dwarfs, or ...
Chapter21
... disk instability — A possible explanation for the origin of a close pair of stars in which one star forms within the disk of gas and dust orbiting another, newly formed, star. eclipsing binary — Binary star systems for which the orbital plane of the stars lies so nearly in the line of sight that two ...
... disk instability — A possible explanation for the origin of a close pair of stars in which one star forms within the disk of gas and dust orbiting another, newly formed, star. eclipsing binary — Binary star systems for which the orbital plane of the stars lies so nearly in the line of sight that two ...
Supernovae: Heavy Elements
... spectral class and luminosity. Some stars can be distinguished from one spectral class to another with the naked eye. • Main Sequence stars generally run from lower right (low temperature and luminosity) to upper left (high temperature and luminosity) • Exceptions - Secondary band of very cool, yet ...
... spectral class and luminosity. Some stars can be distinguished from one spectral class to another with the naked eye. • Main Sequence stars generally run from lower right (low temperature and luminosity) to upper left (high temperature and luminosity) • Exceptions - Secondary band of very cool, yet ...
Formation of Stars
... wavelengths. Infrared and radio waves pass through dust because their wavelengths are much larger than the size of a typical dust particle. ...
... wavelengths. Infrared and radio waves pass through dust because their wavelengths are much larger than the size of a typical dust particle. ...
AmiraPoster3
... • Our raw value for Ko and the corresponding upper limit on the neutron star mass, 1.020.10 Mסּ, are both comparable with those found by van der Meer et al. (2005). • Previous studies assume the giant star is Roche-lobe filling, thus giving only upper limits to the stellar masses. • Effects of X-r ...
... • Our raw value for Ko and the corresponding upper limit on the neutron star mass, 1.020.10 Mסּ, are both comparable with those found by van der Meer et al. (2005). • Previous studies assume the giant star is Roche-lobe filling, thus giving only upper limits to the stellar masses. • Effects of X-r ...
Solution Sheet Lab 1
... Purpose. To determine the length of the sidereal day (the “star” day) from an image of the circumpolar region of the sky. The length of the sidereal day is defined as the time interval between two successive transits of the vernal equinox across the meridian. It is time based upon the Earth’s rotati ...
... Purpose. To determine the length of the sidereal day (the “star” day) from an image of the circumpolar region of the sky. The length of the sidereal day is defined as the time interval between two successive transits of the vernal equinox across the meridian. It is time based upon the Earth’s rotati ...
Ch 28 Class Notes
... 2. An important class of pulsating stars are called _____________________________. These are yellow supergiants whose cycles of brightness range from about 1 day to 50 days (5 is average). The absolute magnitude of a Cepheid is related to the length of time between its periods of maximum brightness ...
... 2. An important class of pulsating stars are called _____________________________. These are yellow supergiants whose cycles of brightness range from about 1 day to 50 days (5 is average). The absolute magnitude of a Cepheid is related to the length of time between its periods of maximum brightness ...
Astronomy 102, Spring 2003 Solutions to Review Problems
... For an older supernova, where you see the expanding gasses of a supernova remnant, if you find a pulsar at the center of the remnant, you know it was a core collapse supernova. A pulsar is a rotating neutron star, and a neutron star is what’s left behind (usually) from the core collapse of a Type II ...
... For an older supernova, where you see the expanding gasses of a supernova remnant, if you find a pulsar at the center of the remnant, you know it was a core collapse supernova. A pulsar is a rotating neutron star, and a neutron star is what’s left behind (usually) from the core collapse of a Type II ...
doc - EU-HOU
... You will fit your measurements by hand. In order to do this, iteratively change the 3 parameters W, T and Phi ( checking the fit (the red points and curve superimposed on the blue points) by eye after each iteration. It is also possible to find the best fit by minimising the “solver” value1 displ ...
... You will fit your measurements by hand. In order to do this, iteratively change the 3 parameters W, T and Phi ( checking the fit (the red points and curve superimposed on the blue points) by eye after each iteration. It is also possible to find the best fit by minimising the “solver” value1 displ ...
Lecture 13 (pdf from the powerpoint)
... • The length of time a star spends fusing hydrogen into helium is called its main sequence lifetime ...
... • The length of time a star spends fusing hydrogen into helium is called its main sequence lifetime ...
ASTR 5340: Radio Astronomy Problem Set 1 Due: 13 September
... The star Betelgeuse is an excellent candidate. Betelgeuse (aka α Orionis because it is the brightest star visible in the Orion constellation) is the red star that defines the left shoulder of Orion. It is an extremely luminous (bolometric luminosity L ≈ 105 L⊙ , where the ⊙ subscript refers to the S ...
... The star Betelgeuse is an excellent candidate. Betelgeuse (aka α Orionis because it is the brightest star visible in the Orion constellation) is the red star that defines the left shoulder of Orion. It is an extremely luminous (bolometric luminosity L ≈ 105 L⊙ , where the ⊙ subscript refers to the S ...
Star - Uplift Education
... Binary star is a stellar system consisting of two stars orbiting around their common center of mass. The ONLY way to find mass of the stars is when they are the part of binary stars. Knowing the period of the binary and the separation of the stars the total mass of the binary system can be calculat ...
... Binary star is a stellar system consisting of two stars orbiting around their common center of mass. The ONLY way to find mass of the stars is when they are the part of binary stars. Knowing the period of the binary and the separation of the stars the total mass of the binary system can be calculat ...
ppt - Serbian Virtual Observatory - astronomical observatory belgrade
... A double star is more general than a binary. To form a binary a star pair must be gravitationally bound. Consequently, to establish the nature means to examine if a given pair is gravitationally bound or, at least, how probable this is. Why probable, because of data lack, very often the data body i ...
... A double star is more general than a binary. To form a binary a star pair must be gravitationally bound. Consequently, to establish the nature means to examine if a given pair is gravitationally bound or, at least, how probable this is. Why probable, because of data lack, very often the data body i ...
Cygnus (constellation)
Cygnus /ˈsɪɡnəs/ is a northern constellation lying on the plane of the Milky Way, deriving its name from the Latinized Greek word for swan. The swan is one of the most recognizable constellations of the northern summer and autumn, it features a prominent asterism known as the Northern Cross (in contrast to the Southern Cross). Cygnus was among the 48 constellations listed by the 2nd century astronomer Ptolemy, and it remains one of the 88 modern constellations.Cygnus contains Deneb, one of the brightest stars in the night sky and one corner of the Summer Triangle, as well as some notable X-ray sources and the giant stellar association of Cygnus OB2. One of the stars of this association, NML Cygni, is one of the largest stars currently known. The constellation is also home to Cygnus X-1, a distant X-ray binary containing a supergiant and unseen massive companion that was the first object widely held to be a black hole. Many star systems in Cygnus have known planets as a result of the Kepler Mission observing one patch of the sky, the patch is the area around Cygnus. In addition, most of the eastern part of Cygnus is dominated by the Hercules–Corona Borealis Great Wall, a giant galaxy filament that is the largest known structure in the observable universe; covering most of the northern sky.