F03HW08
... hot enough to sustain nuclear fusion. The temperature of the interior of the sun decreases from the center to the photosphere. At that point the temperature will be lower than is required to cause the nuclei to approach each other with sufficient energy to overcome the coulomb repulsion. Therefore, ...
... hot enough to sustain nuclear fusion. The temperature of the interior of the sun decreases from the center to the photosphere. At that point the temperature will be lower than is required to cause the nuclei to approach each other with sufficient energy to overcome the coulomb repulsion. Therefore, ...
Homework Solutions: Chapter 7, The Sun
... Q: What evidence do we have that corona has a very high temperature? A: The spectral emission lines of the corona are strongly broadened in wavelength, indicating extremely high temperature. Furthermore in the corona’s spectrum we find emission lines of highly ionized gases which also give us more e ...
... Q: What evidence do we have that corona has a very high temperature? A: The spectral emission lines of the corona are strongly broadened in wavelength, indicating extremely high temperature. Furthermore in the corona’s spectrum we find emission lines of highly ionized gases which also give us more e ...
Stellar Astronomy Sample Questions for Exam 3
... 1. Explain why the distance to some stars can be determined by parallax but most stellar distances cannot. 2. Describe the different properties of main sequence stars that are determined by the mass of the star. Why is mass so important to the characteristics of a star? 3. Why is it so important to ...
... 1. Explain why the distance to some stars can be determined by parallax but most stellar distances cannot. 2. Describe the different properties of main sequence stars that are determined by the mass of the star. Why is mass so important to the characteristics of a star? 3. Why is it so important to ...
Bluffing your way in Astronomy: Taurus
... shine light into space, so it still ends up brighter than the Sun. It’s a old star too, being much further through its lifecycle than the Sun, having exhausted its supply of hydrogen it is now generating energy by fusing atoms of helium into carbon. In other words, it isn’t too well and is on the st ...
... shine light into space, so it still ends up brighter than the Sun. It’s a old star too, being much further through its lifecycle than the Sun, having exhausted its supply of hydrogen it is now generating energy by fusing atoms of helium into carbon. In other words, it isn’t too well and is on the st ...
File
... Earth’s orbit around the Sun is determined by the balance of the Sun’s gravitational pull on Earth and Earth’s forward momentum as it travels around the Sun. Without the Sun’s gravitational pull, Earth would not move in a circle around the Sun, but would continue moving in a straight line through th ...
... Earth’s orbit around the Sun is determined by the balance of the Sun’s gravitational pull on Earth and Earth’s forward momentum as it travels around the Sun. Without the Sun’s gravitational pull, Earth would not move in a circle around the Sun, but would continue moving in a straight line through th ...
Astronomical Numbers
... flat earth under a domed sky. 3) From Earth, stars appear to move in circles around Polaris, the North Star. ...
... flat earth under a domed sky. 3) From Earth, stars appear to move in circles around Polaris, the North Star. ...
Hall Scorpius constellation (11) Jacob Hall Physics 1040, sec 002
... is the same color as the planet Mars. Antares is a red supergiant with a radius about 800 times that of the Sun. It is classified as a variable star; its apparent magnitude varies between 0.9 and 1.8. It has a hot blue companion star about 2.9 arcseconds away. (2) Antares is the 16th brightest star ...
... is the same color as the planet Mars. Antares is a red supergiant with a radius about 800 times that of the Sun. It is classified as a variable star; its apparent magnitude varies between 0.9 and 1.8. It has a hot blue companion star about 2.9 arcseconds away. (2) Antares is the 16th brightest star ...
Exploring the Universe
... microwaves that are emitted all over the sky i. Scientists believe that these microwaves are the remains of the radiation produced during the Big ...
... microwaves that are emitted all over the sky i. Scientists believe that these microwaves are the remains of the radiation produced during the Big ...
Chapter 13 The Life of a Star The Life of a Star Mass Is the Key The
... • Stars smaller than 0.1 M rarely seen since their mass is too small for their cores to initiate fusion reactions • Objects with masses between planets and are called brown dwarfs, “failed stars” extremely dim and difficult to observe • Upper mass limit of stars (about 30 M) due to extreme tempera ...
... • Stars smaller than 0.1 M rarely seen since their mass is too small for their cores to initiate fusion reactions • Objects with masses between planets and are called brown dwarfs, “failed stars” extremely dim and difficult to observe • Upper mass limit of stars (about 30 M) due to extreme tempera ...
17_LectureOutline
... Measuring Stellar Masses in Binary Stars In order to measure stellar masses in a binary star, the period and semimajor axis of the orbit must be measured. Once this is done, Kepler’s third law gives the sum of the masses of the two stars. Then the relative speeds of the two stars can be measured usi ...
... Measuring Stellar Masses in Binary Stars In order to measure stellar masses in a binary star, the period and semimajor axis of the orbit must be measured. Once this is done, Kepler’s third law gives the sum of the masses of the two stars. Then the relative speeds of the two stars can be measured usi ...
Slide 1
... Measuring Stellar Masses in Binary Stars In order to measure stellar masses in a binary star, the period and semimajor axis of the orbit must be measured. Once this is done, Kepler’s third law gives the sum of the masses of the two stars. Then the relative speeds of the two stars can be measured usi ...
... Measuring Stellar Masses in Binary Stars In order to measure stellar masses in a binary star, the period and semimajor axis of the orbit must be measured. Once this is done, Kepler’s third law gives the sum of the masses of the two stars. Then the relative speeds of the two stars can be measured usi ...
Spectroscopic parallax
... The relationship between a Cepheid variable's luminosity and variability period is quite precise, and has been used as a standard candle (astronomical object that has a know luminosity) for almost a century. This connection was discovered in 1912 by Henrietta Swan Leavitt. She measured the brightnes ...
... The relationship between a Cepheid variable's luminosity and variability period is quite precise, and has been used as a standard candle (astronomical object that has a know luminosity) for almost a century. This connection was discovered in 1912 by Henrietta Swan Leavitt. She measured the brightnes ...
Chapter 13
... • Intense outward gas flows from surfaces • Occupy H-R diagram just above main-sequence ...
... • Intense outward gas flows from surfaces • Occupy H-R diagram just above main-sequence ...
Death of Stars notes
... • The SOFIA finding demonstrates that supernovas not only produce dust, but that the dust can survive the explosion to become raw material for the formation of other stars—and planets. • This result supports the notion that most of the dust observed in distant young galaxies may have been made by su ...
... • The SOFIA finding demonstrates that supernovas not only produce dust, but that the dust can survive the explosion to become raw material for the formation of other stars—and planets. • This result supports the notion that most of the dust observed in distant young galaxies may have been made by su ...
Lecture 15, PPT version
... At their maximum brightness, supernovae are as bright as an entire galaxy. ...
... At their maximum brightness, supernovae are as bright as an entire galaxy. ...
Interpreting the HR diagram of stellar clusters
... In fact, it seems that stars are usually born in big groups, as members of a cluster of stars. All the stars in the cluster form at about the same time. So, if we look at a cluster, we see a bunch of stars which are all roughly the same age. However, the stars do not all have the same mass: most ten ...
... In fact, it seems that stars are usually born in big groups, as members of a cluster of stars. All the stars in the cluster form at about the same time. So, if we look at a cluster, we see a bunch of stars which are all roughly the same age. However, the stars do not all have the same mass: most ten ...
Astronomy 122 mid Term Exam
... 9. We observe a binary star system in which both stars have the same physical age. However, one of these stars is a 10 solar mass main sequence star while its companion is a 1 solar mass white dwarf. Explain what is odd about this system and provide a plausible explanation for this apparently parado ...
... 9. We observe a binary star system in which both stars have the same physical age. However, one of these stars is a 10 solar mass main sequence star while its companion is a 1 solar mass white dwarf. Explain what is odd about this system and provide a plausible explanation for this apparently parado ...
Document
... – Low-mass stars have higher density. • High-mass protostars become stars relatively quickly. – They contract quickly due to stronger gravity. – Core becomes hot enough for fusion at a lower ...
... – Low-mass stars have higher density. • High-mass protostars become stars relatively quickly. – They contract quickly due to stronger gravity. – Core becomes hot enough for fusion at a lower ...
Stars - Mike Brotherton
... Remnants of stars with ~ 1 – a few Msun Radii: R ~ 0.2 - 3 light years Expanding at ~10 – 20 km/s ( Doppler shifts) Less than 10,000 years old Have nothing to do with planets! ...
... Remnants of stars with ~ 1 – a few Msun Radii: R ~ 0.2 - 3 light years Expanding at ~10 – 20 km/s ( Doppler shifts) Less than 10,000 years old Have nothing to do with planets! ...
Celestial Distances
... To infer the luminosity, mass, and size of a star from observations (as in a celestial census), we need to know the distance to the star How can we measure the great distances to stars? We use various techniques, useful at different scales, with each scale connecting to the next, like a ladder On th ...
... To infer the luminosity, mass, and size of a star from observations (as in a celestial census), we need to know the distance to the star How can we measure the great distances to stars? We use various techniques, useful at different scales, with each scale connecting to the next, like a ladder On th ...
The Ancient Heavens: Exploring the History of Astronomy
... and Pawnee constellations can help students to understand that all cultures depended on knowing the stars and constellations. ...
... and Pawnee constellations can help students to understand that all cultures depended on knowing the stars and constellations. ...
Figure 1
... sources (stars, clusters, and blended objects) for each galaxy., including locations, photometric uncertainties, and sizes. For each galaxy, a catalog of cluster ages, masses, extinction, and uncertainties, as derived from multi-band SED fitting (both deterministic and stochastic cluster models). ...
... sources (stars, clusters, and blended objects) for each galaxy., including locations, photometric uncertainties, and sizes. For each galaxy, a catalog of cluster ages, masses, extinction, and uncertainties, as derived from multi-band SED fitting (both deterministic and stochastic cluster models). ...
Corvus (constellation)
Corvus is a small constellation in the Southern Celestial Hemisphere. Its name comes from the Latin word ""raven"" or ""crow"". It includes only 11 stars with brighter than 4.02 magnitudes. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations. The four brightest stars, Gamma, Delta, Epsilon, and Beta Corvi from a distinctive quadrilateral in the night sky. The young star Eta Corvi has been found to have two debris disks.