AST1100 Lecture Notes
... stars range from 0.08M⊙ for the least massive stars up to about 100M⊙ for the most massive stars. We will later discuss theoretical arguments explaining why there is a lower and an upper limit of star masses. We will now start to look at the evolution of stars, from birth to death. Stars start out a ...
... stars range from 0.08M⊙ for the least massive stars up to about 100M⊙ for the most massive stars. We will later discuss theoretical arguments explaining why there is a lower and an upper limit of star masses. We will now start to look at the evolution of stars, from birth to death. Stars start out a ...
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... any signs of SF taking place there. The disc component is made up of spiral arms where young stars are forming even now, as it is gas rich. This is where we find open star clusters which are looser aggregates of stars with typical lifetimes of a few 100 Myr1 . The nuclear bulge contains the highest ...
... any signs of SF taking place there. The disc component is made up of spiral arms where young stars are forming even now, as it is gas rich. This is where we find open star clusters which are looser aggregates of stars with typical lifetimes of a few 100 Myr1 . The nuclear bulge contains the highest ...
ASTRONOMY 120
... hydrogen lines. A Type-II supernova results from the collapse of the iron core of a single supermassive star. The star first collapses inward, and then “rebounds” outward. Since most of the star is hydrogen and helium, the spectrum of a Type-II supernova will have strong lines from these elements. T ...
... hydrogen lines. A Type-II supernova results from the collapse of the iron core of a single supermassive star. The star first collapses inward, and then “rebounds” outward. Since most of the star is hydrogen and helium, the spectrum of a Type-II supernova will have strong lines from these elements. T ...
Gravitational redshifts
... synthetic line profiles) are shorter than laboratory values due to convective blueshift. Curves before and after mid-transit (µ = 0.21, 0.59, 0.87) are not exact mirror images due to intrinsic stellar line asymmetries. This simulation from a CO5BOLD model predicts the behavior of an Fe I line ( 620 ...
... synthetic line profiles) are shorter than laboratory values due to convective blueshift. Curves before and after mid-transit (µ = 0.21, 0.59, 0.87) are not exact mirror images due to intrinsic stellar line asymmetries. This simulation from a CO5BOLD model predicts the behavior of an Fe I line ( 620 ...
Chapter 12 Star Stuff How do stars form?
... The relationship between apparent brightness and luminosity depends on distance: ...
... The relationship between apparent brightness and luminosity depends on distance: ...
Lecture 20: Formation of Planets, Exoplanets 3/30
... Planets in other Star Systems first extrasolar planet observed in 1995. In Jan 2000, 28 observed and now about 3700 confirmed. Many systems with 2 or more observed planets • difficult to observe directly • mostly look for impact on Star: wobbles due to gravity of planets or reduction of light due t ...
... Planets in other Star Systems first extrasolar planet observed in 1995. In Jan 2000, 28 observed and now about 3700 confirmed. Many systems with 2 or more observed planets • difficult to observe directly • mostly look for impact on Star: wobbles due to gravity of planets or reduction of light due t ...
Stellar Evolution – Cosmic Cycles of Formation and Destruction
... further, becoming cooler and redder. Giant stars fuse elements up to carbon. Most of these stars go through a Mira variable instability stage with a periodicity of ~80 - 1000 days. Stars that have evolved to the giant branch are commonly referred to as red giants. Eventually these red giants will sh ...
... further, becoming cooler and redder. Giant stars fuse elements up to carbon. Most of these stars go through a Mira variable instability stage with a periodicity of ~80 - 1000 days. Stars that have evolved to the giant branch are commonly referred to as red giants. Eventually these red giants will sh ...
Falling Stars
... hundreds of stars falling every minute! All night, the sky was brightened by meteors that rocketed through the night by the thousands! Since no telescopes or fancy equipment were needed to see the storm, ordinary people were able to see that wonderful and rare sight. Many artists tried to paint pict ...
... hundreds of stars falling every minute! All night, the sky was brightened by meteors that rocketed through the night by the thousands! Since no telescopes or fancy equipment were needed to see the storm, ordinary people were able to see that wonderful and rare sight. Many artists tried to paint pict ...
Lecture 12, PPT version
... Galaxy). All of the stars formed at roughly the same time. Globular clusters have lots of RED stars, but no BLUE stars (because they died long ago and were not “replenished”). ...
... Galaxy). All of the stars formed at roughly the same time. Globular clusters have lots of RED stars, but no BLUE stars (because they died long ago and were not “replenished”). ...
The Star Finder Book - Starpath School of Navigation
... Under cloudy skies, the extreme value of accurate dead reckoning becomes clear very soon. But this is not the subject at hand, and improving dead reckoning procedure is easily accommodated underway without special training. The problem with cloudy skies we cover here is that of identifying unknown s ...
... Under cloudy skies, the extreme value of accurate dead reckoning becomes clear very soon. But this is not the subject at hand, and improving dead reckoning procedure is easily accommodated underway without special training. The problem with cloudy skies we cover here is that of identifying unknown s ...
Stars: Their Life and Afterlife
... pressure. Having thrown off their outer layers of hydrogen and helium in thermal pulses (forming a so-called “planetary nebula” around the star), these stars become white dwarfs – exposed, hot carbon-oxygen cores that slowly radiate their stored heat energy and cool. We will discuss white dwarfs mor ...
... pressure. Having thrown off their outer layers of hydrogen and helium in thermal pulses (forming a so-called “planetary nebula” around the star), these stars become white dwarfs – exposed, hot carbon-oxygen cores that slowly radiate their stored heat energy and cool. We will discuss white dwarfs mor ...
The Solar Neighborhood
... Since brighter stars are designated with a smaller number for apparent magnitude, magnitudes are plotted in reverse order to put the brighter stars at the top. Investigating Stellar Evolution - For each cluster, identify the main sequence, and sketch in a line that follows the main sequence from its ...
... Since brighter stars are designated with a smaller number for apparent magnitude, magnitudes are plotted in reverse order to put the brighter stars at the top. Investigating Stellar Evolution - For each cluster, identify the main sequence, and sketch in a line that follows the main sequence from its ...
Astrophysics * Glossary - Uplift Summit International
... where R is the radius of the star, A it’s surface area, T it’s surface temperature, and σ is the Stefan-Boltzmann constant. █ State one factor that determines the luminosity of a star • mass / temperature / surface area / radius / type of star / composition █ Describe what is meant by apparent brigh ...
... where R is the radius of the star, A it’s surface area, T it’s surface temperature, and σ is the Stefan-Boltzmann constant. █ State one factor that determines the luminosity of a star • mass / temperature / surface area / radius / type of star / composition █ Describe what is meant by apparent brigh ...
Lyra
Lyra (/ˈlaɪərə/; Latin for lyre, from Greek λύρα) is a small constellation. It is one of 48 listed by the 2nd century astronomer Ptolemy, and is one of the 88 constellations recognized by the International Astronomical Union. Lyra was often represented on star maps as a vulture or an eagle carrying a lyre, and hence sometimes referred to as Aquila Cadens or Vultur Cadens. Beginning at the north, Lyra is bordered by Draco, Hercules, Vulpecula, and Cygnus. Lyra is visible from the northern hemisphere from spring through autumn, and nearly overhead, in temperate latitudes, during the summer months. From the southern hemisphere, it is visible low in the northern sky during the winter months.The lucida or brightest star—and one of the brightest stars in the sky—is the white main sequence star Vega, a corner of the Summer Triangle. Beta Lyrae is the prototype of a class of stars known as Beta Lyrae variables, binary stars so close to each other that they become egg-shaped and material flows from one to the other. Epsilon Lyrae, known informally as the Double Double, is a complex multiple star system. Lyra also hosts the Ring Nebula, the second-discovered and best-known planetary nebula.