Slide 1
... • P. 8.6 Compute your Schwarz radius and density for BH of your mass. – If an object shrinks to the Schwarzschild Radius it will ultimately collapse to a singularity (basically vanish from our universe). A singularity is like what happens to 1/x when x0. Eq. 8.8 is: RS =2GM/c^2 (Example 8.2 did RS w ...
... • P. 8.6 Compute your Schwarz radius and density for BH of your mass. – If an object shrinks to the Schwarzschild Radius it will ultimately collapse to a singularity (basically vanish from our universe). A singularity is like what happens to 1/x when x0. Eq. 8.8 is: RS =2GM/c^2 (Example 8.2 did RS w ...
Slide 1
... •Ellipticals have lots of globular clusters (about twice that of disk galaxies) •these fall into two groups based on color •color determined by metallicity, with more metal-rich GCs (redder) possibly the result of galaxy mergers •Ellipticals have much less cool, atomic gas than spiral galaxies •< 1 ...
... •Ellipticals have lots of globular clusters (about twice that of disk galaxies) •these fall into two groups based on color •color determined by metallicity, with more metal-rich GCs (redder) possibly the result of galaxy mergers •Ellipticals have much less cool, atomic gas than spiral galaxies •< 1 ...
Measuring Radii and Temperatures of Stars
... • To avoid uncertainties in Teff and BC • Determine PV as a function of B-V PV(B-V)=logTeff – 0.1BC PV ( B V ) a b( B V ) c( B V ) 2 d ( B V )3 ...
... • To avoid uncertainties in Teff and BC • Determine PV as a function of B-V PV(B-V)=logTeff – 0.1BC PV ( B V ) a b( B V ) c( B V ) 2 d ( B V )3 ...
Integrated Science
... times that of our Sun. This means that a neutron star is so dense that on Earth, one teaspoonful would weigh a billion tons! Because of its small size and high density, a neutron star possesses a surface gravitational field about 2 x 1011 times that of Earth. Neutron stars can also have magnetic fie ...
... times that of our Sun. This means that a neutron star is so dense that on Earth, one teaspoonful would weigh a billion tons! Because of its small size and high density, a neutron star possesses a surface gravitational field about 2 x 1011 times that of Earth. Neutron stars can also have magnetic fie ...
The Night Sky
... Binary stars with radii bigger than their Roche lobe cannot form. How then can binary stars transfer matter between them? ...
... Binary stars with radii bigger than their Roche lobe cannot form. How then can binary stars transfer matter between them? ...
astronomy timeline
... Annie J. Cannon and co-workers present thousands of stellar spectral classifications in the Henry Draper Catalogue. Cannon and her co-workers devised a classification system for stellar spectra and used it to produce a catalog of spectra classifications for about 225,000 stars. p. 368-370, F 12.9 ...
... Annie J. Cannon and co-workers present thousands of stellar spectral classifications in the Henry Draper Catalogue. Cannon and her co-workers devised a classification system for stellar spectra and used it to produce a catalog of spectra classifications for about 225,000 stars. p. 368-370, F 12.9 ...
Power-point slides for Lecture 5
... as we shall see. And the boundary pressure of the overlying silicon shell is not entirely negligible. ...
... as we shall see. And the boundary pressure of the overlying silicon shell is not entirely negligible. ...
Constellations - Brown University Wiki
... seven sisters, a cluster of six bright stars ( about 200 in a telescope) known all over the world but now counted as part of the larger group called the constellation Taurus (the Bull) and the asterism “the Big Dipper”, the seven brightest stars in the larger group called Ursa Major (the Big Bear). ...
... seven sisters, a cluster of six bright stars ( about 200 in a telescope) known all over the world but now counted as part of the larger group called the constellation Taurus (the Bull) and the asterism “the Big Dipper”, the seven brightest stars in the larger group called Ursa Major (the Big Bear). ...
Friday, April 25 - Otterbein University
... • The orbital plane of the pair almost edge-on to our line of sight • We observe periodic changes in the starlight as one member of the binary passes in front of the other ...
... • The orbital plane of the pair almost edge-on to our line of sight • We observe periodic changes in the starlight as one member of the binary passes in front of the other ...
Comments from John Saunders.
... distance is kilometres is 415,500,000,000,000 or 415.5 trillion km’s. It has been estimated that it would take approximately 50,000 years for our fastest spacecraft to-date to reach Alpha Centauri. It’s not like popping over for a cup of tea….and this is our nearest star. Although when we look up at ...
... distance is kilometres is 415,500,000,000,000 or 415.5 trillion km’s. It has been estimated that it would take approximately 50,000 years for our fastest spacecraft to-date to reach Alpha Centauri. It’s not like popping over for a cup of tea….and this is our nearest star. Although when we look up at ...
Lecture 1
... angle formula to estimate the linear distance between two dots on the screen. They all sat in the same seat while making the measurements. Will there be a bias in their measurements? ...
... angle formula to estimate the linear distance between two dots on the screen. They all sat in the same seat while making the measurements. Will there be a bias in their measurements? ...
The Milky Way as a Spiral galaxy
... From the motions of stars in the galaxy, and the 21-cm data, we know that the galaxy rotates. The Sun takes ~250 million years to complete one orbit around the galactic center. The inner stars complete their orbits in shorter times. This differential rotation would destroy the spiral arms though, w ...
... From the motions of stars in the galaxy, and the 21-cm data, we know that the galaxy rotates. The Sun takes ~250 million years to complete one orbit around the galactic center. The inner stars complete their orbits in shorter times. This differential rotation would destroy the spiral arms though, w ...
Cosmic Dawn A Hunting for the First Stars in the Universe
... the resulting heat of compression. Otherwise, restorative gas pressure will halt gravitational collapse well before the gas can reach the temperatures and densities required to sustain nuclear fusion. No stars could ever be born in this scenario. Fortunately, there are ways around the problem via mo ...
... the resulting heat of compression. Otherwise, restorative gas pressure will halt gravitational collapse well before the gas can reach the temperatures and densities required to sustain nuclear fusion. No stars could ever be born in this scenario. Fortunately, there are ways around the problem via mo ...
PDF - BYU Studies
... pass away. Modern astrophysics teaches that stars are formed, enjoy an enormously long “summer” as they fuse hydrogen to helium in their core, then undergo major changes as nuclear fuel runs low, and finally fade away (occasionally with grand fireworks). The sun is enjoying its glorious summer, but ...
... pass away. Modern astrophysics teaches that stars are formed, enjoy an enormously long “summer” as they fuse hydrogen to helium in their core, then undergo major changes as nuclear fuel runs low, and finally fade away (occasionally with grand fireworks). The sun is enjoying its glorious summer, but ...
COM 2014 January
... King Acrisius of Argos was warned by an oracle that one day he would be killed by his own grandson. To prevent any likelihood of this ever happening, he locked away his beautiful daughter, Danae, so that no man could ever reach her. But this did not stop the god Zeus, with his fondness for mortal wo ...
... King Acrisius of Argos was warned by an oracle that one day he would be killed by his own grandson. To prevent any likelihood of this ever happening, he locked away his beautiful daughter, Danae, so that no man could ever reach her. But this did not stop the god Zeus, with his fondness for mortal wo ...
IK Pegasi
IK Pegasi (or HR 8210) is a binary star system in the constellation Pegasus. It is just luminous enough to be seen with the unaided eye, at a distance of about 150 light years from the Solar System.The primary (IK Pegasi A) is an A-type main-sequence star that displays minor pulsations in luminosity. It is categorized as a Delta Scuti variable star and it has a periodic cycle of luminosity variation that repeats itself about 22.9 times per day. Its companion (IK Pegasi B) is a massive white dwarf—a star that has evolved past the main sequence and is no longer generating energy through nuclear fusion. They orbit each other every 21.7 days with an average separation of about 31 million kilometres, or 19 million miles, or 0.21 astronomical units (AU). This is smaller than the orbit of Mercury around the Sun.IK Pegasi B is the nearest known supernova progenitor candidate. When the primary begins to evolve into a red giant, it is expected to grow to a radius where the white dwarf can accrete matter from the expanded gaseous envelope. When the white dwarf approaches the Chandrasekhar limit of 1.44 solar masses (M☉), it may explode as a Type Ia supernova.