Sarbani Basu and William J. Chaplin
- Published in print:
- 2017
- Published Online:
- May 2018
- ISBN:
- 9780691162928
- eISBN:
- 9781400888207
- Item type:
- chapter
- Publisher:
- Princeton University Press
- DOI:
- 10.23943/princeton/9780691162928.003.0007
- Subject:
- Physics, Particle Physics / Astrophysics / Cosmology
This chapter determines stellar properties from seismic data. It discusses how the average seismic properties discussed in the previous chapters are used in determining the mass and radius of a star. ...
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This chapter determines stellar properties from seismic data. It discusses how the average seismic properties discussed in the previous chapters are used in determining the mass and radius of a star. The chapter provides two ways of determining stellar properties: the “direct method” and grid-based modeling. The first method produces a set of model-independent results derived from a set of equations. On the other hand, the grid-based model, which can make up for the shortcomings of the direct method, derives its results from a fairly dense grid of stellar models of different metallicities that cover a wide range of masses and evolutionary stages.Less
This chapter determines stellar properties from seismic data. It discusses how the average seismic properties discussed in the previous chapters are used in determining the mass and radius of a star. The chapter provides two ways of determining stellar properties: the “direct method” and grid-based modeling. The first method produces a set of model-independent results derived from a set of equations. On the other hand, the grid-based model, which can make up for the shortcomings of the direct method, derives its results from a fairly dense grid of stellar models of different metallicities that cover a wide range of masses and evolutionary stages.
John Chambers and Jacqueline Mitton
- Published in print:
- 2017
- Published Online:
- May 2018
- ISBN:
- 9780691175706
- eISBN:
- 9781400885565
- Item type:
- chapter
- Publisher:
- Princeton University Press
- DOI:
- 10.23943/princeton/9780691175706.003.0007
- Subject:
- History, History of Science, Technology, and Medicine
This chapter focuses on the nature and composition of the Milky Way galaxy. The main component of the Milky Way is a rotating disk of stars some 100,000 light-years across but only about 1,000 ...
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This chapter focuses on the nature and composition of the Milky Way galaxy. The main component of the Milky Way is a rotating disk of stars some 100,000 light-years across but only about 1,000 light-years thick. Between the stars lies an extremely tenuous mixture of gas and fine dust grains called the interstellar medium. The disk of stars is only about 1,000 light-years thick but becomes thicker near the Milky Way's center, where a bar-shaped bulge of densely packed stars surrounds a supermassive black hole at the heart of the galaxy. Enveloping the thin stellar disk is an extended disk of gas about 10 times thicker. Today, stars are forming in the Milky Way at a rate equivalent to one solar-mass star every year. Judging by the age of its oldest members, the Milky Way has been giving birth to new stars for over 13 billion years.Less
This chapter focuses on the nature and composition of the Milky Way galaxy. The main component of the Milky Way is a rotating disk of stars some 100,000 light-years across but only about 1,000 light-years thick. Between the stars lies an extremely tenuous mixture of gas and fine dust grains called the interstellar medium. The disk of stars is only about 1,000 light-years thick but becomes thicker near the Milky Way's center, where a bar-shaped bulge of densely packed stars surrounds a supermassive black hole at the heart of the galaxy. Enveloping the thin stellar disk is an extended disk of gas about 10 times thicker. Today, stars are forming in the Milky Way at a rate equivalent to one solar-mass star every year. Judging by the age of its oldest members, the Milky Way has been giving birth to new stars for over 13 billion years.
