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 ...
Unit 3 - Lesson 8.9 Life of Stars Challenge
... These large stars have diameters between 10X and 100X that of the Sun. If the star is a Super Giant, their diameters can be up to 1000X of the Sun. A late-life stage sub-species star that emits a beam of electromagnetic radiation that can be only seen when the beam of emission is pointing toward the ...
... These large stars have diameters between 10X and 100X that of the Sun. If the star is a Super Giant, their diameters can be up to 1000X of the Sun. A late-life stage sub-species star that emits a beam of electromagnetic radiation that can be only seen when the beam of emission is pointing toward the ...
Plotting Variable Stars on the H
... Miras and Cepheids are especially elongated because of these expansions and contractions. Some pulsating variable stars change in temperature by two spectral classes during one cycle of change from maximum to minimum. To better understand the degree of variation for individual variable stars, it is ...
... Miras and Cepheids are especially elongated because of these expansions and contractions. Some pulsating variable stars change in temperature by two spectral classes during one cycle of change from maximum to minimum. To better understand the degree of variation for individual variable stars, it is ...
Amanda Boyle Starstuff
... black holes and they drag everything down with themselves. But stellar collisions are not so common, at least to us because the universe operates in billions of years, and as a result our fleeting existence makes it difficult to speak with authority on these things. But we do understand the mainstr ...
... black holes and they drag everything down with themselves. But stellar collisions are not so common, at least to us because the universe operates in billions of years, and as a result our fleeting existence makes it difficult to speak with authority on these things. But we do understand the mainstr ...
Diffuse Ultraviolet Emission in Galaxies
... P Cygni’s spectrum is quite unlike that of most stars. Typically, a stellar spectrum will feature numerous dark “absorption” lines, which are produced by atoms in its outer layers absorbing certain wavelengths of light emitted from below. A star’s spectrum may also exhibit bright “emission” lines—th ...
... P Cygni’s spectrum is quite unlike that of most stars. Typically, a stellar spectrum will feature numerous dark “absorption” lines, which are produced by atoms in its outer layers absorbing certain wavelengths of light emitted from below. A star’s spectrum may also exhibit bright “emission” lines—th ...
CHAPTER 30: STARS, GALAXIES AND THE UNIVERSE Analyzing
... Stars vary in size and mass. Stars such as our sun are considered medium-sized stars. The sun has a diameter of 1,390,000 km. Most of the stars you can see in the night sky are medium-sized stars. Many stars also have about the same mass as the sun, however some stars may be more or less massive. St ...
... Stars vary in size and mass. Stars such as our sun are considered medium-sized stars. The sun has a diameter of 1,390,000 km. Most of the stars you can see in the night sky are medium-sized stars. Many stars also have about the same mass as the sun, however some stars may be more or less massive. St ...
upperMS - CWRU Astronomy
... OBN stars come from mass loss in OB stars Say the CN cycle converts CN in the inner 60% of a star over 15% of its main sequence lifetime If 40% of the remaining mass can be removed in the final 85% of the lifetime, then it’s a nitrogen rich star It’s ok to lose this much mass and still be OB, but i ...
... OBN stars come from mass loss in OB stars Say the CN cycle converts CN in the inner 60% of a star over 15% of its main sequence lifetime If 40% of the remaining mass can be removed in the final 85% of the lifetime, then it’s a nitrogen rich star It’s ok to lose this much mass and still be OB, but i ...
Lecture 8a Star Formation 10/15/2014
... • Stars are formed from interstellar material which is compressed by gravity • Spend >90% of their lives burning Hydrogen into Helium • How they “die” depends on mass " large stars blow up Supernovas • Understand stars’ lifecycles by studying their properties and also groups of stars ...
... • Stars are formed from interstellar material which is compressed by gravity • Spend >90% of their lives burning Hydrogen into Helium • How they “die” depends on mass " large stars blow up Supernovas • Understand stars’ lifecycles by studying their properties and also groups of stars ...
Stars - CBSD.org
... Magnitudes • Hipparchus decided that all the brightest stars in the night sky were “first order magnitude” stars. • As they got dimmer, he classified them as “second magnitude,” “third magnitude,” and so on… • He got up to magnitude 6, after which stars are too dim to be seen without a telescope. • ...
... Magnitudes • Hipparchus decided that all the brightest stars in the night sky were “first order magnitude” stars. • As they got dimmer, he classified them as “second magnitude,” “third magnitude,” and so on… • He got up to magnitude 6, after which stars are too dim to be seen without a telescope. • ...
The Abundances of the Fe Group Elements in Three Early B Stars in
... The abundances of C and N are good indicators of the chemical evolution in a galaxy. The FUSE spectral region contains several lines of carbon and nitrogen, including resonance lines of C III and N III. The latter are not good for analysis as they are blended with the ISM features. In Fig. 4 we show ...
... The abundances of C and N are good indicators of the chemical evolution in a galaxy. The FUSE spectral region contains several lines of carbon and nitrogen, including resonance lines of C III and N III. The latter are not good for analysis as they are blended with the ISM features. In Fig. 4 we show ...
Astronomy Report Southern Cross Authors Maria Constanza Pavez
... very simple to explain. In Antiquity people used fantastic stories that helped to explain the origin of all the surrounding phenomena, and in so doing many civilizations mentioned the Southern Cross in their myths and legends. Many of them explain us about the ancient location of the constellation. ...
... very simple to explain. In Antiquity people used fantastic stories that helped to explain the origin of all the surrounding phenomena, and in so doing many civilizations mentioned the Southern Cross in their myths and legends. Many of them explain us about the ancient location of the constellation. ...
Notes
... Zanstra temperature - Measure brightness of star compared to brightness of nebula in optical hydrogen emission lines to estimate the uv/optical flux ratio to get temperature ...
... Zanstra temperature - Measure brightness of star compared to brightness of nebula in optical hydrogen emission lines to estimate the uv/optical flux ratio to get temperature ...
star
... The Lives of Stars Stars live for a very long time, up to 100 million years or more No humans can possibly observe a star this long! How can we learn about the stages in a star’s life? We can take a celestial census, getting a snapshot of many stars at different stages of their life We can then try ...
... The Lives of Stars Stars live for a very long time, up to 100 million years or more No humans can possibly observe a star this long! How can we learn about the stages in a star’s life? We can take a celestial census, getting a snapshot of many stars at different stages of their life We can then try ...
Stars part 1
... 2. Luminosity – the total amount of energy a star radiates each second. Luminosity of all visible stars range from 1/1,000,000 the luminosity of the sun to 1,000,000 time the luminosity of the sun. 90% of the stars are not as bright as the sun. ...
... 2. Luminosity – the total amount of energy a star radiates each second. Luminosity of all visible stars range from 1/1,000,000 the luminosity of the sun to 1,000,000 time the luminosity of the sun. 90% of the stars are not as bright as the sun. ...
Time From the Perspective of a Particle Physicist
... Radius • Find that some are related Large Mass Large Brightness • Determine model of stellar formation and life cycle ...
... Radius • Find that some are related Large Mass Large Brightness • Determine model of stellar formation and life cycle ...
Stars, Galaxies, and the Universe Section 1 Distances to Stars
... • 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 ...
Auriga (constellation)
Auriga is one of the 48 constellations listed by the 2nd-century astronomer Ptolemy and remains one of the 88 modern constellations. Located north of the celestial equator, its name is the Latin word for ""charioteer"", associating it with various mythological charioteers, including Erichthonius and Myrtilus. Auriga is most prominent during winter evenings in the Northern Hemisphere, along with the five other constellations that have stars in the Winter Hexagon asterism. Because of its northern declination, Auriga is only visible in its entirety as far as 34° south; for observers farther south it lies partially or fully below the horizon. A large constellation, with an area of 657 square degrees, it is half the size of the largest constellation, Hydra.Its brightest star, Capella, is an unusual multiple star system among the brightest stars in the night sky. Beta Aurigae is an interesting variable star in the constellation; Epsilon Aurigae, a nearby eclipsing binary with an unusually long period, has been studied intensively. Because of its position near the winter Milky Way, Auriga has many bright open clusters in its borders, including M36, M37, and M38, popular targets for amateur astronomers. In addition, it has one prominent nebula, the Flaming Star Nebula, associated with the variable star AE Aurigae.In Chinese mythology, Auriga's stars were incorporated into several constellations, including the celestial emperors' chariots, made up of the modern constellation's brightest stars. Auriga is home to the radiant for the Aurigids, Zeta Aurigids, Delta Aurigids, and the hypothesized Iota Aurigids.