Astronomy Assignment #1
... collapsing core is pushed deeper into the star as the core collapses and can now fuse for the first time. Shell Hburning begins. The shell H-burning releases gamma rays that do not have to thermalize out of the core so they hit the envelope with more energy that core gamma rays would and, in effect, ...
... collapsing core is pushed deeper into the star as the core collapses and can now fuse for the first time. Shell Hburning begins. The shell H-burning releases gamma rays that do not have to thermalize out of the core so they hit the envelope with more energy that core gamma rays would and, in effect, ...
Problem 4: magnitude of the star?
... index B-V=0 are all characteristics of stars with spectral type A. A0 B. B0 C. F0 D. G0 E. K0 __C___13. A star forms on the main sequence with twice the mass of our sun. It’s lifetime on the main sequence, relative to that for a solar mass star, is A. The same B. Half as long C. 1/4 as long D. 1/9 a ...
... index B-V=0 are all characteristics of stars with spectral type A. A0 B. B0 C. F0 D. G0 E. K0 __C___13. A star forms on the main sequence with twice the mass of our sun. It’s lifetime on the main sequence, relative to that for a solar mass star, is A. The same B. Half as long C. 1/4 as long D. 1/9 a ...
A Star is “Born,” and then How Will it Move
... Young (Embedded) Clusters: Very young (<10 Myr-old) groups of young stars that form together. Future binding depends on cluster mass & velocity, seems that 90% dissolve before ~10 Myr (Lada & Lada 2003). When they unbind but are still seen to move together, they’re known as a “stellar association.” ...
... Young (Embedded) Clusters: Very young (<10 Myr-old) groups of young stars that form together. Future binding depends on cluster mass & velocity, seems that 90% dissolve before ~10 Myr (Lada & Lada 2003). When they unbind but are still seen to move together, they’re known as a “stellar association.” ...
Chapter 16 - "The Universe"
... – The second stage begins when the hydrogen core becomes fused to produce helium. • As there are now less hydrogen fusion reactions, less energy is produced, which means less outward pressure, so the star begins to collapse due to gravitational pull. • This collapse begins to heat the helium core o ...
... – The second stage begins when the hydrogen core becomes fused to produce helium. • As there are now less hydrogen fusion reactions, less energy is produced, which means less outward pressure, so the star begins to collapse due to gravitational pull. • This collapse begins to heat the helium core o ...
Star Formation
... Galaxy 2) Stars are “born” in dense, cold, interstellar clouds (giant molecular clouds) 3) Star formation is triggered when the cloud is compressed ...
... Galaxy 2) Stars are “born” in dense, cold, interstellar clouds (giant molecular clouds) 3) Star formation is triggered when the cloud is compressed ...
The Milky Way
... stars in our Milky Way are not single stars, but belong to binaries: Pairs or multiple systems of stars which orbit their common center of mass. If we can measure and understand their orbital motion, we can estimate the stellar ...
... stars in our Milky Way are not single stars, but belong to binaries: Pairs or multiple systems of stars which orbit their common center of mass. If we can measure and understand their orbital motion, we can estimate the stellar ...
Lecture 12, PPT version
... Spherical groupings of 10,000 to 1 million stars (about 158 known in our 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”). ...
... Spherical groupings of 10,000 to 1 million stars (about 158 known in our 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”). ...
ASTRONOMY 120
... Roughly how big (in A.U.) will the Sun become when it enters the red-giant phase? (3 points) A star like the Sun will evolve into a red giant with a size about 100 times its current size. This is equivalent to about 70 million km, or almost half an AU. 5. Chaisson Review and Discussion 20.8 Do all s ...
... Roughly how big (in A.U.) will the Sun become when it enters the red-giant phase? (3 points) A star like the Sun will evolve into a red giant with a size about 100 times its current size. This is equivalent to about 70 million km, or almost half an AU. 5. Chaisson Review and Discussion 20.8 Do all s ...
Slide 1
... Red Giant phase with inert He-core and outer H-burning shell; star expands and cools, but is brighter Climbs up the RG branch until He-flash in the core Core expands and cools; H-burning decreases; outer layers contract; luminosity decreases but temperature increases; star moves LEFT on the H-R diag ...
... Red Giant phase with inert He-core and outer H-burning shell; star expands and cools, but is brighter Climbs up the RG branch until He-flash in the core Core expands and cools; H-burning decreases; outer layers contract; luminosity decreases but temperature increases; star moves LEFT on the H-R diag ...
January 2006
... stored heat, not by nuclear reactions • core continues to cool and contract • Size ~ Earth • Density: a million times that of Earth – 1 cubic cm has 1000 kg of mass! ...
... stored heat, not by nuclear reactions • core continues to cool and contract • Size ~ Earth • Density: a million times that of Earth – 1 cubic cm has 1000 kg of mass! ...
The Birth, Life, and Death of Stars
... ... for his discovery of the law of the photoelectric effect 1905 Einstein’s Miracle Year while working as a patent clerk in Bern Culmination of the “Special Theory of Relativity” (E = mc 2 ) Revises fundamental Newtonian concepts of space and time 1915: Einstein’s General Theory of Relativity Revis ...
... ... for his discovery of the law of the photoelectric effect 1905 Einstein’s Miracle Year while working as a patent clerk in Bern Culmination of the “Special Theory of Relativity” (E = mc 2 ) Revises fundamental Newtonian concepts of space and time 1915: Einstein’s General Theory of Relativity Revis ...
CHAP
... - The stars’ colors reveal the ____________________ of the stars. - Cool stars appear _________ in color with a surface temperature of about 3,200 degrees Celsius. - Warm stars appear _____________ in color with a surface temperature of about 5,500 degrees Celsius. - The hottest stars are __________ ...
... - The stars’ colors reveal the ____________________ of the stars. - Cool stars appear _________ in color with a surface temperature of about 3,200 degrees Celsius. - Warm stars appear _____________ in color with a surface temperature of about 5,500 degrees Celsius. - The hottest stars are __________ ...
Star Classification
... The ancient Greeks thought this group of stars looked like a hunter, so they named it Orion after their mythical hunter. The line of three stars at the center is "Orion’s Belt." The many different colors of stars reflect the star’s temperature. The bright, red star in the upper left (with an arrow p ...
... The ancient Greeks thought this group of stars looked like a hunter, so they named it Orion after their mythical hunter. The line of three stars at the center is "Orion’s Belt." The many different colors of stars reflect the star’s temperature. The bright, red star in the upper left (with an arrow p ...
test - Scioly.org
... B) Its notable spirals include the Milly Way, M31, and M33. C) Most of its members are dwarf eltiptical and iregular gataxies. D) It contains the large radio galaxy Centaurus A. E) It is about three million light years across. 62) What is the nearest huge cluster ofthousands of galaxies, to which th ...
... B) Its notable spirals include the Milly Way, M31, and M33. C) Most of its members are dwarf eltiptical and iregular gataxies. D) It contains the large radio galaxy Centaurus A. E) It is about three million light years across. 62) What is the nearest huge cluster ofthousands of galaxies, to which th ...
Neutron Star - Perry Local Schools
... from the star’s center, and cooler gas sinks toward the center. – During radiation, atoms absorb energy and transfer it to other atoms in random directions. Atoms near the star’s surface radiate energy into space. ...
... from the star’s center, and cooler gas sinks toward the center. – During radiation, atoms absorb energy and transfer it to other atoms in random directions. Atoms near the star’s surface radiate energy into space. ...
Distances farther out
... 5.3 K lines and chromospheres: Chromosphere: Low density, hot gaseous region (above the higher density photosphere, where the continuum and bulk of absorption lines form). Chromospheres detected by high resolution spectroscopy of strongest lines. Eg. Fraunhofer H & K lines of Ca II (H line of Ca II ...
... 5.3 K lines and chromospheres: Chromosphere: Low density, hot gaseous region (above the higher density photosphere, where the continuum and bulk of absorption lines form). Chromospheres detected by high resolution spectroscopy of strongest lines. Eg. Fraunhofer H & K lines of Ca II (H line of Ca II ...
File
... 2. Which star would most likely be the brightest? Explain your answer. 3. Which star is most similar to our Sun? Explain your answer. ...
... 2. Which star would most likely be the brightest? Explain your answer. 3. Which star is most similar to our Sun? Explain your answer. ...
SAMPLE TEST: Stars and Galaxies Multiple Choice Identify the letter
... 52. Stars that radiate short pulses of radio energy are called ____________________. 53. The most dense stars known to exist are called ____________________. 54. The average star spends ____________________ percent of its life as a hydrogen-burning, main-sequence star. 55. The sun is positioned abou ...
... 52. Stars that radiate short pulses of radio energy are called ____________________. 53. The most dense stars known to exist are called ____________________. 54. The average star spends ____________________ percent of its life as a hydrogen-burning, main-sequence star. 55. The sun is positioned abou ...
Star
A star is a luminous sphere of plasma held together by its own gravity. The nearest star to Earth is the Sun. Other stars are visible from Earth during the night, appearing as a multitude of fixed luminous points in the sky due to their immense distance from Earth. Historically, the most prominent stars were grouped into constellations and asterisms, and the brightest stars gained proper names. Extensive catalogues of stars have been assembled by astronomers, which provide standardized star designations.For at least a portion of its life, a star shines due to thermonuclear fusion of hydrogen into helium in its core, releasing energy that traverses the star's interior and then radiates into outer space. Once the hydrogen in the core of a star is nearly exhausted, almost all naturally occurring elements heavier than helium are created by stellar nucleosynthesis during the star's lifetime and, for some stars, by supernova nucleosynthesis when it explodes. Near the end of its life, a star can also contain degenerate matter. Astronomers can determine the mass, age, metallicity (chemical composition), and many other properties of a star by observing its motion through space, luminosity, and spectrum respectively. The total mass of a star is the principal determinant of its evolution and eventual fate. Other characteristics of a star, including diameter and temperature, change over its life, while the star's environment affects its rotation and movement. A plot of the temperature of many stars against their luminosities, known as a Hertzsprung–Russell diagram (H–R diagram), allows the age and evolutionary state of a star to be determined.A star's life begins with the gravitational collapse of a gaseous nebula of material composed primarily of hydrogen, along with helium and trace amounts of heavier elements. Once the stellar core is sufficiently dense, hydrogen becomes steadily converted into helium through nuclear fusion, releasing energy in the process. The remainder of the star's interior carries energy away from the core through a combination of radiative and convective processes. The star's internal pressure prevents it from collapsing further under its own gravity. Once the hydrogen fuel at the core is exhausted, a star with at least 0.4 times the mass of the Sun expands to become a red giant, in some cases fusing heavier elements at the core or in shells around the core. The star then evolves into a degenerate form, recycling a portion of its matter into the interstellar environment, where it will contribute to the formation of a new generation of stars with a higher proportion of heavy elements. Meanwhile, the core becomes a stellar remnant: a white dwarf, a neutron star, or (if it is sufficiently massive) a black hole.Binary and multi-star systems consist of two or more stars that are gravitationally bound, and generally move around each other in stable orbits. When two such stars have a relatively close orbit, their gravitational interaction can have a significant impact on their evolution. Stars can form part of a much larger gravitationally bound structure, such as a star cluster or a galaxy.