User:Tohline/Apps/HayashiNaritaMiyama82 - Revision history

Tohline: /* See Also */

2019-07-05T17:26:30Z

Tohline: /* See Also */

2019-07-05T17:23:42Z

Tohline at 16:22, 1 July 2019

2019-07-01T16:22:19Z

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			__FORCETOC__

			=Rotationally Flattened Isothermal Structures=
	{{LSU_HBook_header}}		{{LSU_HBook_header}}

	~~=Rotationally Flattened Isothermal Structures=~~
	[[Image:LSU_Structure_still.gif\|74px\|left]]		[[Image:LSU_Structure_still.gif\|74px\|left]]
	[https://ui.adsabs.harvard.edu/abs/1982PThPh..68.1949H/abstract Hayashi, Narita & Miyama] (1982; hereafter HNM82) discovered an analytic solution to the equations that govern the structure of rotationally flattened, self-gravitating isothermal gas clouds. Their solution describes a family of centrally condensed models whose degree of flattening ranges from a spherical structure to an infinitesimally thin disk. For several reasons, I consider this to be one of the most remarkable discoveries — and, hence, one of the most significant papers — related to the structure of self-gravitating systems that was published in the decade of the '80s. First, as has been [[User:Tohline/Apps/MaclaurinSpheroids#Maclaurin_Spheroids_(axisymmetric_structure)\|remarked earlier]], there is no particular reason why one should guess ahead of time that the equilibrium properties of ''any'' rotating, self-gravitating configuration should be describable in terms of analytic functions. When dealing with compressible equations of state, such analytic solutions are rare even in the context of spherically symmetric structures, so it is impressive that HNM82 found a solution for rotationally flattened, isothermal configurations. Second, about six months earlier the same year, [https://ui.adsabs.harvard.edu/abs/1982ApJ...259..535T/abstract Alar Toomre (1982)] published an independent discovery and strikingly independent derivation of exactly the same family of rotationally flattened, isothermal models.<sup>1</sup> Third, these two independent derivations were motivated by a desire to better understand two quite different astrophysical environments: The research of HNM82 was focused on star-forming gas clouds while Toomre's research was focused on the structure of elliptical galaxies and the dark-matter halos around spiral galaxies.		[https://ui.adsabs.harvard.edu/abs/1982PThPh..68.1949H/abstract Hayashi, Narita & Miyama] (1982; hereafter HNM82) discovered an analytic solution to the equations that govern the structure of rotationally flattened, self-gravitating isothermal gas clouds. Their solution describes a family of centrally condensed models whose degree of flattening ranges from a spherical structure to an infinitesimally thin disk. For several reasons, I consider this to be one of the most remarkable discoveries — and, hence, one of the most significant papers — related to the structure of self-gravitating systems that was published in the decade of the '80s. First, as has been [[User:Tohline/Apps/MaclaurinSpheroids#Maclaurin_Spheroids_(axisymmetric_structure)\|remarked earlier]], there is no particular reason why one should guess ahead of time that the equilibrium properties of ''any'' rotating, self-gravitating configuration should be describable in terms of analytic functions. When dealing with compressible equations of state, such analytic solutions are rare even in the context of spherically symmetric structures, so it is impressive that HNM82 found a solution for rotationally flattened, isothermal configurations. Second, about six months earlier the same year, [https://ui.adsabs.harvard.edu/abs/1982ApJ...259..535T/abstract Alar Toomre (1982)] published an independent discovery and strikingly independent derivation of exactly the same family of rotationally flattened, isothermal models.<sup>1</sup> Third, these two independent derivations were motivated by a desire to better understand two quite different astrophysical environments: The research of HNM82 was focused on star-forming gas clouds while Toomre's research was focused on the structure of elliptical galaxies and the dark-matter halos around spiral galaxies.

Tohline: /* Structural Properties */

2019-06-26T21:05:02Z

Structural Properties

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	<table border="1" align="center" cellpadding="5" width="420px">		<table border="1" align="center" cellpadding="5" width="420px">
	<tr>		<tr>
	<th align="center">3D Renderings of Isothermal Disks from [~~http~~://adsabs.harvard.edu/abs/1982PThPh..68.1949H Hayashi, Narita & Miyama (1982)]</th>		<th align="center">3D Renderings of Isothermal Disks from [https://ui.adsabs.harvard.edu/abs/1982PThPh..68.1949H/abstract Hayashi, Narita & Miyama (1982)]</th>
	</tr>		</tr>
	<tr><td align="center">		<tr><td align="center">

Tohline: /* Rotationally Flattened Isothermal Structures */

2019-06-26T21:04:39Z

Rotationally Flattened Isothermal Structures

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	=Rotationally Flattened Isothermal Structures=		=Rotationally Flattened Isothermal Structures=
	[[Image:LSU_Structure_still.gif\|74px\|left]]		[[Image:LSU_Structure_still.gif\|74px\|left]]
	[~~http~~://adsabs.harvard.edu/abs/1982PThPh..68.1949H Hayashi, Narita & Miyama] (1982; hereafter HNM82) discovered an analytic solution to the equations that govern the structure of rotationally flattened, self-gravitating isothermal gas clouds. Their solution describes a family of centrally condensed models whose degree of flattening ranges from a spherical structure to an infinitesimally thin disk. For several reasons, I consider this to be one of the most remarkable discoveries — and, hence, one of the most significant papers — related to the structure of self-gravitating systems that was published in the decade of the '80s. First, as has been [[User:Tohline/Apps/MaclaurinSpheroids#Maclaurin_Spheroids_(axisymmetric_structure)\|remarked earlier]], there is no particular reason why one should guess ahead of time that the equilibrium properties of ''any'' rotating, self-gravitating configuration should be describable in terms of analytic functions. When dealing with compressible equations of state, such analytic solutions are rare even in the context of spherically symmetric structures, so it is impressive that HNM82 found a solution for rotationally flattened, isothermal configurations. Second, about six months earlier the same year, [https://ui.adsabs.harvard.edu/abs/1982ApJ...259..535T/abstract Alar Toomre (1982)] published an independent discovery and strikingly independent derivation of exactly the same family of rotationally flattened, isothermal models.<sup>1</sup> Third, these two independent derivations were motivated by a desire to better understand two quite different astrophysical environments: The research of HNM82 was focused on star-forming gas clouds while Toomre's research was focused on the structure of elliptical galaxies and the dark-matter halos around spiral galaxies.		[https://ui.adsabs.harvard.edu/abs/1982PThPh..68.1949H/abstract Hayashi, Narita & Miyama] (1982; hereafter HNM82) discovered an analytic solution to the equations that govern the structure of rotationally flattened, self-gravitating isothermal gas clouds. Their solution describes a family of centrally condensed models whose degree of flattening ranges from a spherical structure to an infinitesimally thin disk. For several reasons, I consider this to be one of the most remarkable discoveries — and, hence, one of the most significant papers — related to the structure of self-gravitating systems that was published in the decade of the '80s. First, as has been [[User:Tohline/Apps/MaclaurinSpheroids#Maclaurin_Spheroids_(axisymmetric_structure)\|remarked earlier]], there is no particular reason why one should guess ahead of time that the equilibrium properties of ''any'' rotating, self-gravitating configuration should be describable in terms of analytic functions. When dealing with compressible equations of state, such analytic solutions are rare even in the context of spherically symmetric structures, so it is impressive that HNM82 found a solution for rotationally flattened, isothermal configurations. Second, about six months earlier the same year, [https://ui.adsabs.harvard.edu/abs/1982ApJ...259..535T/abstract Alar Toomre (1982)] published an independent discovery and strikingly independent derivation of exactly the same family of rotationally flattened, isothermal models.<sup>1</sup> Third, these two independent derivations were motivated by a desire to better understand two quite different astrophysical environments: The research of HNM82 was focused on star-forming gas clouds while Toomre's research was focused on the structure of elliptical galaxies and the dark-matter halos around spiral galaxies.

	Despite my assertion that HNM82 is one of the most significant papers to be published over the past few decades, citation indexes reveal that it is not widely referenced. In large part I attribute this to the fact that HNM82 was published in a Japanese journal ([https://academic.oup.com/ptp ''Progress of Theoretical Physics'']) that has only fairly recently made its archival articles available to the open-access, [https://ui.adsabs.harvard.edu Astrophysics Data System].		Despite my assertion that HNM82 is one of the most significant papers to be published over the past few decades, citation indexes reveal that it is not widely referenced. In large part I attribute this to the fact that HNM82 was published in a Japanese journal ([https://academic.oup.com/ptp ''Progress of Theoretical Physics'']) that has only fairly recently made its archival articles available to the open-access, [https://ui.adsabs.harvard.edu Astrophysics Data System].

Tohline: /* Rotationally Flattened Isothermal Structures */

2019-06-26T21:01:23Z

Rotationally Flattened Isothermal Structures

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	[http://adsabs.harvard.edu/abs/1982PThPh..68.1949H Hayashi, Narita & Miyama] (1982; hereafter HNM82) discovered an analytic solution to the equations that govern the structure of rotationally flattened, self-gravitating isothermal gas clouds. Their solution describes a family of centrally condensed models whose degree of flattening ranges from a spherical structure to an infinitesimally thin disk. For several reasons, I consider this to be one of the most remarkable discoveries — and, hence, one of the most significant papers — related to the structure of self-gravitating systems that was published in the decade of the '80s. First, as has been [[User:Tohline/Apps/MaclaurinSpheroids#Maclaurin_Spheroids_(axisymmetric_structure)\|remarked earlier]], there is no particular reason why one should guess ahead of time that the equilibrium properties of ''any'' rotating, self-gravitating configuration should be describable in terms of analytic functions. When dealing with compressible equations of state, such analytic solutions are rare even in the context of spherically symmetric structures, so it is impressive that HNM82 found a solution for rotationally flattened, isothermal configurations. Second, about six months earlier the same year, [https://ui.adsabs.harvard.edu/abs/1982ApJ...259..535T/abstract Alar Toomre (1982)] published an independent discovery and strikingly independent derivation of exactly the same family of rotationally flattened, isothermal models.<sup>1</sup> Third, these two independent derivations were motivated by a desire to better understand two quite different astrophysical environments: The research of HNM82 was focused on star-forming gas clouds while Toomre's research was focused on the structure of elliptical galaxies and the dark-matter halos around spiral galaxies.		[http://adsabs.harvard.edu/abs/1982PThPh..68.1949H Hayashi, Narita & Miyama] (1982; hereafter HNM82) discovered an analytic solution to the equations that govern the structure of rotationally flattened, self-gravitating isothermal gas clouds. Their solution describes a family of centrally condensed models whose degree of flattening ranges from a spherical structure to an infinitesimally thin disk. For several reasons, I consider this to be one of the most remarkable discoveries — and, hence, one of the most significant papers — related to the structure of self-gravitating systems that was published in the decade of the '80s. First, as has been [[User:Tohline/Apps/MaclaurinSpheroids#Maclaurin_Spheroids_(axisymmetric_structure)\|remarked earlier]], there is no particular reason why one should guess ahead of time that the equilibrium properties of ''any'' rotating, self-gravitating configuration should be describable in terms of analytic functions. When dealing with compressible equations of state, such analytic solutions are rare even in the context of spherically symmetric structures, so it is impressive that HNM82 found a solution for rotationally flattened, isothermal configurations. Second, about six months earlier the same year, [https://ui.adsabs.harvard.edu/abs/1982ApJ...259..535T/abstract Alar Toomre (1982)] published an independent discovery and strikingly independent derivation of exactly the same family of rotationally flattened, isothermal models.<sup>1</sup> Third, these two independent derivations were motivated by a desire to better understand two quite different astrophysical environments: The research of HNM82 was focused on star-forming gas clouds while Toomre's research was focused on the structure of elliptical galaxies and the dark-matter halos around spiral galaxies.

	Despite my assertion that HNM82 is one of the most significant papers to be published over the past few decades, citation indexes reveal that it is not widely referenced. In large part I attribute this to the fact that HNM82 was published in a Japanese journal ([~~http~~://~~ptp~~.~~ipap~~.~~jp/journal~~/ ''Progress of Theoretical Physics'']) that has only fairly recently made its archival articles available to the open-access, [https://ui.adsabs.harvard.edu Astrophysics Data System].		Despite my assertion that HNM82 is one of the most significant papers to be published over the past few decades, citation indexes reveal that it is not widely referenced. In large part I attribute this to the fact that HNM82 was published in a Japanese journal ([https://academic.oup.com/ptp ''Progress of Theoretical Physics'']) that has only fairly recently made its archival articles available to the open-access, [https://ui.adsabs.harvard.edu Astrophysics Data System].

	==Governing Relations==		==Governing Relations==

Tohline: /* Rotationally Flattened Isothermal Structures */

2019-06-26T20:59:28Z

Rotationally Flattened Isothermal Structures

← Older revision		Revision as of 20:59, 26 June 2019
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	[http://adsabs.harvard.edu/abs/1982PThPh..68.1949H Hayashi, Narita & Miyama] (1982; hereafter HNM82) discovered an analytic solution to the equations that govern the structure of rotationally flattened, self-gravitating isothermal gas clouds. Their solution describes a family of centrally condensed models whose degree of flattening ranges from a spherical structure to an infinitesimally thin disk. For several reasons, I consider this to be one of the most remarkable discoveries — and, hence, one of the most significant papers — related to the structure of self-gravitating systems that was published in the decade of the '80s. First, as has been [[User:Tohline/Apps/MaclaurinSpheroids#Maclaurin_Spheroids_(axisymmetric_structure)\|remarked earlier]], there is no particular reason why one should guess ahead of time that the equilibrium properties of ''any'' rotating, self-gravitating configuration should be describable in terms of analytic functions. When dealing with compressible equations of state, such analytic solutions are rare even in the context of spherically symmetric structures, so it is impressive that HNM82 found a solution for rotationally flattened, isothermal configurations. Second, about six months earlier the same year, [https://ui.adsabs.harvard.edu/abs/1982ApJ...259..535T/abstract Alar Toomre (1982)] published an independent discovery and strikingly independent derivation of exactly the same family of rotationally flattened, isothermal models.<sup>1</sup> Third, these two independent derivations were motivated by a desire to better understand two quite different astrophysical environments: The research of HNM82 was focused on star-forming gas clouds while Toomre's research was focused on the structure of elliptical galaxies and the dark-matter halos around spiral galaxies.		[http://adsabs.harvard.edu/abs/1982PThPh..68.1949H Hayashi, Narita & Miyama] (1982; hereafter HNM82) discovered an analytic solution to the equations that govern the structure of rotationally flattened, self-gravitating isothermal gas clouds. Their solution describes a family of centrally condensed models whose degree of flattening ranges from a spherical structure to an infinitesimally thin disk. For several reasons, I consider this to be one of the most remarkable discoveries — and, hence, one of the most significant papers — related to the structure of self-gravitating systems that was published in the decade of the '80s. First, as has been [[User:Tohline/Apps/MaclaurinSpheroids#Maclaurin_Spheroids_(axisymmetric_structure)\|remarked earlier]], there is no particular reason why one should guess ahead of time that the equilibrium properties of ''any'' rotating, self-gravitating configuration should be describable in terms of analytic functions. When dealing with compressible equations of state, such analytic solutions are rare even in the context of spherically symmetric structures, so it is impressive that HNM82 found a solution for rotationally flattened, isothermal configurations. Second, about six months earlier the same year, [https://ui.adsabs.harvard.edu/abs/1982ApJ...259..535T/abstract Alar Toomre (1982)] published an independent discovery and strikingly independent derivation of exactly the same family of rotationally flattened, isothermal models.<sup>1</sup> Third, these two independent derivations were motivated by a desire to better understand two quite different astrophysical environments: The research of HNM82 was focused on star-forming gas clouds while Toomre's research was focused on the structure of elliptical galaxies and the dark-matter halos around spiral galaxies.

	Despite my assertion that HNM82 is one of the most significant papers to be published over the past few decades, citation indexes reveal that it is not widely referenced. In large part I attribute this to the fact that HNM82 was published in a Japanese journal ([http://ptp.ipap.jp/journal/ ''Progress of Theoretical Physics'']) that has only fairly recently made its archival articles available to the open-access, [~~http~~://~~www~~.adsabs.harvard.edu/ Astrophysics Data System].		Despite my assertion that HNM82 is one of the most significant papers to be published over the past few decades, citation indexes reveal that it is not widely referenced. In large part I attribute this to the fact that HNM82 was published in a Japanese journal ([http://ptp.ipap.jp/journal/ ''Progress of Theoretical Physics'']) that has only fairly recently made its archival articles available to the open-access, [https://ui.adsabs.harvard.edu Astrophysics Data System].

	==Governing Relations==		==Governing Relations==

Tohline: /* Rotationally Flattened Isothermal Structures */

2019-06-26T20:58:29Z

Rotationally Flattened Isothermal Structures

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	=Rotationally Flattened Isothermal Structures=		=Rotationally Flattened Isothermal Structures=
	[[Image:LSU_Structure_still.gif\|74px\|left]]		[[Image:LSU_Structure_still.gif\|74px\|left]]
	[http://adsabs.harvard.edu/abs/1982PThPh..68.1949H Hayashi, Narita & Miyama] (1982; hereafter HNM82) discovered an analytic solution to the equations that govern the structure of rotationally flattened, self-gravitating isothermal gas clouds. Their solution describes a family of centrally condensed models whose degree of flattening ranges from a spherical structure to an infinitesimally thin disk. For several reasons, I consider this to be one of the most remarkable discoveries — and, hence, one of the most significant papers — related to the structure of self-gravitating systems that was published in the decade of the '80s. First, as has been [[User:Tohline/Apps/MaclaurinSpheroids#Maclaurin_Spheroids_(axisymmetric_structure)\|remarked earlier]], there is no particular reason why one should guess ahead of time that the equilibrium properties of ''any'' rotating, self-gravitating configuration should be describable in terms of analytic functions. When dealing with compressible equations of state, such analytic solutions are rare even in the context of spherically symmetric structures, so it is impressive that HNM82 found a solution for rotationally flattened, isothermal configurations. Second, about six months earlier the same year, [~~http~~://adsabs.harvard.edu/abs/1982ApJ...259..535T Alar Toomre (1982)] published an independent discovery and strikingly independent derivation of exactly the same family of rotationally flattened, isothermal models.<sup>1</sup> Third, these two independent derivations were motivated by a desire to better understand two quite different astrophysical environments: The research of HNM82 was focused on star-forming gas clouds while Toomre's research was focused on the structure of elliptical galaxies and the dark-matter halos around spiral galaxies.		[http://adsabs.harvard.edu/abs/1982PThPh..68.1949H Hayashi, Narita & Miyama] (1982; hereafter HNM82) discovered an analytic solution to the equations that govern the structure of rotationally flattened, self-gravitating isothermal gas clouds. Their solution describes a family of centrally condensed models whose degree of flattening ranges from a spherical structure to an infinitesimally thin disk. For several reasons, I consider this to be one of the most remarkable discoveries — and, hence, one of the most significant papers — related to the structure of self-gravitating systems that was published in the decade of the '80s. First, as has been [[User:Tohline/Apps/MaclaurinSpheroids#Maclaurin_Spheroids_(axisymmetric_structure)\|remarked earlier]], there is no particular reason why one should guess ahead of time that the equilibrium properties of ''any'' rotating, self-gravitating configuration should be describable in terms of analytic functions. When dealing with compressible equations of state, such analytic solutions are rare even in the context of spherically symmetric structures, so it is impressive that HNM82 found a solution for rotationally flattened, isothermal configurations. Second, about six months earlier the same year, [https://ui.adsabs.harvard.edu/abs/1982ApJ...259..535T/abstract Alar Toomre (1982)] published an independent discovery and strikingly independent derivation of exactly the same family of rotationally flattened, isothermal models.<sup>1</sup> Third, these two independent derivations were motivated by a desire to better understand two quite different astrophysical environments: The research of HNM82 was focused on star-forming gas clouds while Toomre's research was focused on the structure of elliptical galaxies and the dark-matter halos around spiral galaxies.

	Despite my assertion that HNM82 is one of the most significant papers to be published over the past few decades, citation indexes reveal that it is not widely referenced. In large part I attribute this to the fact that HNM82 was published in a Japanese journal ([http://ptp.ipap.jp/journal/ ''Progress of Theoretical Physics'']) that has only fairly recently made its archival articles available to the open-access, [http://www.adsabs.harvard.edu/ Astrophysics Data System].		Despite my assertion that HNM82 is one of the most significant papers to be published over the past few decades, citation indexes reveal that it is not widely referenced. In large part I attribute this to the fact that HNM82 was published in a Japanese journal ([http://ptp.ipap.jp/journal/ ''Progress of Theoretical Physics'']) that has only fairly recently made its archival articles available to the open-access, [http://www.adsabs.harvard.edu/ Astrophysics Data System].

Tohline: /* Structural Properties */

2019-06-26T20:55:52Z

Structural Properties

← Older revision		Revision as of 20:55, 26 June 2019
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	<table border="1" align="center" cellpadding="5" width="420px">		<table border="1" align="center" cellpadding="5" width="420px">
	<tr>		<tr>
	<th align="center">3D Renderings of Isothermal Disks from Hayashi, Narita & Miyama (1982)</th>		<th align="center">3D Renderings of Isothermal Disks from [http://adsabs.harvard.edu/abs/1982PThPh..68.1949H Hayashi, Narita & Miyama (1982)]</th>
	</tr>		</tr>
	<tr><td align="center">		<tr><td align="center">

Tohline at 23:00, 15 June 2019

2019-06-15T23:00:07Z

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	#At the end of their paper, HNM82 present the following '''Note added in proof:''' "After we submitted this paper, a paper by Toomre (Astrophys. J. '''259''' (1982), 535) appeared. He also found the same solutions as Eq. (2.3), although he did not study the stability of the equilibrium configurations."		#At the end of their paper, HNM82 present the following '''Note added in proof:''' "After we submitted this paper, a paper by Toomre (Astrophys. J. '''259''' (1982), 535) appeared. He also found the same solutions as Eq. (2.3), although he did not study the stability of the equilibrium configurations."


			=See Also=
			* [https://ui.adsabs.harvard.edu/abs/1987ApJ...317..830K/abstract M. Kiguchi, S. Narita, S. M. Miyama & C. Hayashi (1987)], ApJ, 317, 830: ''The Equilibria of Rotating Isothermal Clouds''
			* [https://ui.adsabs.harvard.edu/abs/1988PThPS..96...50K/abstract M. Kiguchi, S. Narita, S. M. Miyama & C. Hayashi (1988)], Progress in Theoretical Physics, 96, 50: ''Chapter 4. The Equilibrium and the Stability of Rotating Isothermal Clouds''

	<br />		<br />
	{{LSU_HBook_footer}}		{{LSU_HBook_footer}}

← Older revision		Revision as of 17:26, 5 July 2019
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	=See Also=		=See Also=
	* [https://ui.adsabs.harvard.edu/abs/1985A%26A...143..355H/abstract I. Hachisu & Y. Eriguchi (1985)], Astronomy & Astrophysics, 143, 355: ''Equilibrium structures of rotating isothermal gas clouds. I.''		* [https://ui.adsabs.harvard.edu/abs/1985A%26A...143..355H/abstract I. Hachisu & Y. Eriguchi (1985)], Astronomy & Astrophysics, 143, 355: ''Equilibrium structures of rotating isothermal gas clouds. I.''
			* [https://ui.adsabs.harvard.edu/abs/1985A%26A...147...13H/abstract I. Hachisu & Y. Eriguchi (1985)], Astronomy & Astrophysics, 147, 13: ''Equilibrium structures of rotating isothermal gas clouds. II — Dependence on the angular momentum distribution''
	* [https://ui.adsabs.harvard.edu/abs/1987ApJ...317..830K/abstract M. Kiguchi, S. Narita, S. M. Miyama & C. Hayashi (1987)], ApJ, 317, 830: ''The Equilibria of Rotating Isothermal Clouds''		* [https://ui.adsabs.harvard.edu/abs/1987ApJ...317..830K/abstract M. Kiguchi, S. Narita, S. M. Miyama & C. Hayashi (1987)], ApJ, 317, 830: ''The Equilibria of Rotating Isothermal Clouds''
	* [https://ui.adsabs.harvard.edu/abs/1988PThPS..96...50K/abstract M. Kiguchi, S. Narita, S. M. Miyama & C. Hayashi (1988)], Progress in Theoretical Physics, 96, 50: ''Chapter 4. The Equilibrium and the Stability of Rotating Isothermal Clouds''		* [https://ui.adsabs.harvard.edu/abs/1988PThPS..96...50K/abstract M. Kiguchi, S. Narita, S. M. Miyama & C. Hayashi (1988)], Progress in Theoretical Physics, 96, 50: ''Chapter 4. The Equilibrium and the Stability of Rotating Isothermal Clouds''

← Older revision		Revision as of 17:23, 5 July 2019
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	=See Also=		=See Also=
			* [https://ui.adsabs.harvard.edu/abs/1985A%26A...143..355H/abstract I. Hachisu & Y. Eriguchi (1985)], Astronomy & Astrophysics, 143, 355: ''Equilibrium structures of rotating isothermal gas clouds. I.''
	* [https://ui.adsabs.harvard.edu/abs/1987ApJ...317..830K/abstract M. Kiguchi, S. Narita, S. M. Miyama & C. Hayashi (1987)], ApJ, 317, 830: ''The Equilibria of Rotating Isothermal Clouds''		* [https://ui.adsabs.harvard.edu/abs/1987ApJ...317..830K/abstract M. Kiguchi, S. Narita, S. M. Miyama & C. Hayashi (1987)], ApJ, 317, 830: ''The Equilibria of Rotating Isothermal Clouds''
	* [https://ui.adsabs.harvard.edu/abs/1988PThPS..96...50K/abstract M. Kiguchi, S. Narita, S. M. Miyama & C. Hayashi (1988)], Progress in Theoretical Physics, 96, 50: ''Chapter 4. The Equilibrium and the Stability of Rotating Isothermal Clouds''		* [https://ui.adsabs.harvard.edu/abs/1988PThPS..96...50K/abstract M. Kiguchi, S. Narita, S. M. Miyama & C. Hayashi (1988)], Progress in Theoretical Physics, 96, 50: ''Chapter 4. The Equilibrium and the Stability of Rotating Isothermal Clouds''