User:Tohline/Preface - Revision history

Tohline: /* Preface */

2016-11-05T18:10:37Z

Preface

← Older revision		Revision as of 18:10, 5 November 2016
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	In an effort to show the considerable overlap that exists between the discussions presented in this H_Book and the discussions that have appeared previously in the traditional print medium, we have constructed an [http://www.vistrails.org/index.php/User:Tohline/Appendix/Equation_templates appendix containing a set of key physical equations] and, next to each equation, we have identified where this equation is introduced or discussed in each of six published texts. The texts that we have selected are:		In an effort to show the considerable overlap that exists between the discussions presented in this H_Book and the discussions that have appeared previously in the traditional print medium, we have constructed an [http://www.vistrails.org/index.php/User:Tohline/Appendix/Equation_templates appendix containing a set of key physical equations] and, next to each equation, we have identified where this equation is introduced or discussed in each of six published texts. The texts that we have selected are:

	# [<b><font color="red">C67</font></b>] '''Chandrasekhar, S.''' 1967 (originally, 1939), An Introduction to the Study of Stellar Structure (New York: Dover)		* [<b><font color="red">C67</font></b>] '''Chandrasekhar, S.''' 1967 (originally, 1939), An Introduction to the Study of Stellar Structure (New York: Dover)

	# [<b><font color="red">LL75</font></b>] '''Laundau, L. D. & Lifshitz, E. M.''' 1975 (originally, 1959), Fluid Mechanics (New York: Pergamon Press)		* [<b><font color="red">LL75</font></b>] '''Laundau, L. D. & Lifshitz, E. M.''' 1975 (originally, 1959), Fluid Mechanics (New York: Pergamon Press)

	# [<b><font color="red">~~H87~~</font></b>] '''~~Huang~~, K.''' ~~1987 (originally 1963)~~, ~~Statistical Mechanics~~ (New York: John Wiley & Sons)		* [<b><font color="red">ST83</font></b>] <span id="ST83">[http://adsabs.harvard.edu/abs/1983bhwd.book.....S '''Shapiro, S. L. & Teukolsky, S. A.''' 1983],</span> Black Holes, White Dwarfs, and Neutron Stars: The Physics of Compact Objects (New York: John Wiley & Sons); republished in 2004 by WILEY-VCH Verlag GmbH & Co. KGaA

	# [<b><font color="red">~~BT87~~</font></b>] '''~~Binney~~, ~~J. & Tremaine, S~~.''' 1987, ~~Galactic Dynamics~~ (~~Princeton, NJ~~: ~~Princeton University Press~~)		* [<b><font color="red">H87</font></b>] '''Huang, K.''' 1987 (originally 1963), Statistical Mechanics (New York: John Wiley & Sons)

	# [<b><font color="red">~~KW94~~</font></b>] '''~~Kippenhahn~~, R. & ~~Weigert~~, A.''' ~~1994~~, ~~Stellar Structure and Evolution~~ (~~New York~~: ~~Springer-Verlag~~)		* [<b><font color="red">BT87</font></b>] '''Binney, J. & Tremaine, S.''' 1987, Galactic Dynamics (Princeton, NJ: Princeton University Press)

	# [<b><font color="red">P00</font></b>] '''Padmanabhan, T.''' 2000, Theoretical Astrophysics. Volume I: Astrophysical Processes (Cambridge: Cambridge University Press); and Padmanabhan, T. 2001, Theoretical Astrophysics. Volume II: Stars and Stellar Systems (Cambridge: Cambridge University Press)		* [<b><font color="red">KW94</font></b>] '''Kippenhahn, R. & Weigert, A.''' 1994, Stellar Structure and Evolution (New York: Springer-Verlag)

			* [<b><font color="red">P00</font></b>] '''Padmanabhan, T.''' 2000, Theoretical Astrophysics. Volume I: Astrophysical Processes (Cambridge: Cambridge University Press); and Padmanabhan, T. 2001, Theoretical Astrophysics. Volume II: Stars and Stellar Systems (Cambridge: Cambridge University Press)

	The key equations that we have chosen to highlight are drawn from a wide assortment of sub-fields of physics that feed into and, indeed, are essential to our modern understanding of astrophysical systems, including: classical mechanics, fluid dynamics, thermodynamics & statistical mechanics, quantum mechanics, radiation transport, and relativity. Each time one of these equations appears in our discussion, it will be marked as a key equation so that, from the information contained in our [http://www.vistrails.org/index.php/User:Tohline/Appendix/Equation_templates key equations appendix], the reader can be guided to parallel discussions of related concepts as they have been presented in the above-identified, published texts.		The key equations that we have chosen to highlight are drawn from a wide assortment of sub-fields of physics that feed into and, indeed, are essential to our modern understanding of astrophysical systems, including: classical mechanics, fluid dynamics, thermodynamics & statistical mechanics, quantum mechanics, radiation transport, and relativity. Each time one of these equations appears in our discussion, it will be marked as a key equation so that, from the information contained in our [http://www.vistrails.org/index.php/User:Tohline/Appendix/Equation_templates key equations appendix], the reader can be guided to parallel discussions of related concepts as they have been presented in the above-identified, published texts.

Tohline: /* Preface */ Update and complete text references

2010-01-27T17:39:46Z

Preface: Update and complete text references

← Older revision		Revision as of 17:39, 27 January 2010
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	<i>January 24, 2010</i>		<i>January 24, 2010</i>

	In an effort to show the considerable overlap that exists between the discussions presented in this H_Book and the discussions that have appeared previously in the traditional print medium, we have constructed an [http://www.vistrails.org/index.php/User:Tohline/Appendix/Equation_templates appendix containing a set of key physical equations] and, next to each equation, we have identified where this equation is introduced or discussed in each of ~~five different~~ published texts. The texts that we have selected are:		In an effort to show the considerable overlap that exists between the discussions presented in this H_Book and the discussions that have appeared previously in the traditional print medium, we have constructed an [http://www.vistrails.org/index.php/User:Tohline/Appendix/Equation_templates appendix containing a set of key physical equations] and, next to each equation, we have identified where this equation is introduced or discussed in each of six published texts. The texts that we have selected are:
	# Chandrasekhar, S. (~~1967;~~ originally 1939), An Introduction to the Study of Stellar Structure (Dover, New York; originally ~~University of Chicago Press~~, ~~Chicago~~)
	# ~~Landau~~ & ~~Lifschitz~~		# [<b><font color="red">C67</font></b>] '''Chandrasekhar, S.''' 1967 (originally, 1939), An Introduction to the Study of Stellar Structure (New York: Dover)
	# Kippenhahn, R. & Weigert, A. (1994), Stellar Structure and Evolution (Springer-Verlag~~, New York~~)
	# ~~Binney~~, J. ~~& Tremaine~~, S. (~~1989~~), Stellar ~~Dynamics~~ (~~Princeton~~ University Press~~, Princeton~~)		# [<b><font color="red">LL75</font></b>] '''Laundau, L. D. & Lifshitz, E. M.''' 1975 (originally, 1959), Fluid Mechanics (New York: Pergamon Press)

			# [<b><font color="red">H87</font></b>] '''Huang, K.''' 1987 (originally 1963), Statistical Mechanics (New York: John Wiley & Sons)

			# [<b><font color="red">BT87</font></b>] '''Binney, J. & Tremaine, S.''' 1987, Galactic Dynamics (Princeton, NJ: Princeton University Press)

			# [<b><font color="red">KW94</font></b>] '''Kippenhahn, R. & Weigert, A.''' 1994, Stellar Structure and Evolution (New York: Springer-Verlag)

			# [<b><font color="red">P00</font></b>] '''Padmanabhan, T.''' 2000, Theoretical Astrophysics. Volume I: Astrophysical Processes (Cambridge: Cambridge University Press); and Padmanabhan, T. 2001, Theoretical Astrophysics. Volume II: Stars and Stellar Systems (Cambridge: Cambridge University Press)

	The key equations that we have chosen to highlight are drawn from a wide assortment of sub-fields of physics that feed into and, indeed, are essential to our modern understanding of astrophysical systems, including: classical mechanics, fluid dynamics, thermodynamics & statistical mechanics, quantum mechanics, radiation transport, and relativity. Each time one of these equations appears in our discussion, it will be marked as a key equation so that, from the information contained in our [http://www.vistrails.org/index.php/User:Tohline/Appendix/Equation_templates key equations appendix], the reader can be guided to parallel discussions of related concepts as they have been presented in the above-identified, published texts.		The key equations that we have chosen to highlight are drawn from a wide assortment of sub-fields of physics that feed into and, indeed, are essential to our modern understanding of astrophysical systems, including: classical mechanics, fluid dynamics, thermodynamics & statistical mechanics, quantum mechanics, radiation transport, and relativity. Each time one of these equations appears in our discussion, it will be marked as a key equation so that, from the information contained in our [http://www.vistrails.org/index.php/User:Tohline/Appendix/Equation_templates key equations appendix], the reader can be guided to parallel discussions of related concepts as they have been presented in the above-identified, published texts.

Tohline: /* Preface */ Minor rewording of January 2010 preface

2010-01-25T21:49:42Z

Preface: Minor rewording of January 2010 preface

← Older revision		Revision as of 21:49, 25 January 2010
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	<i>January 24, 2010</i>		<i>January 24, 2010</i>

	In an effort to show the considerable overlap that exists between the discussions presented in this H_Book and the discussions that have appeared previously in the traditional print medium, we have constructed an [http://www.vistrails.org/index.php/User:Tohline/Appendix/Equation_templates appendix containing a set of key physical equations] and, next to each equation, we have identified where this equation ~~first appears~~ in each of five different published texts. The texts that we have selected are:		In an effort to show the considerable overlap that exists between the discussions presented in this H_Book and the discussions that have appeared previously in the traditional print medium, we have constructed an [http://www.vistrails.org/index.php/User:Tohline/Appendix/Equation_templates appendix containing a set of key physical equations] and, next to each equation, we have identified where this equation is introduced or discussed in each of five different published texts. The texts that we have selected are:
	# Chandrasekhar, S. (1967; originally 1939), An Introduction to the Study of Stellar Structure (Dover, New York; originally University of Chicago Press, Chicago)		# Chandrasekhar, S. (1967; originally 1939), An Introduction to the Study of Stellar Structure (Dover, New York; originally University of Chicago Press, Chicago)
	# Landau & Lifschitz		# Landau & Lifschitz
	# Kippenhahn, R. & Weigert, A. (1994), Stellar Structure and Evolution (Springer-Verlag, New York)		# Kippenhahn, R. & Weigert, A. (1994), Stellar Structure and Evolution (Springer-Verlag, New York)
	# Binney, J. & Tremaine, S. (1989), Stellar Dynamics (Princeton University Press, Princeton)		# Binney, J. & Tremaine, S. (1989), Stellar Dynamics (Princeton University Press, Princeton)
	The key equations that we have chosen to highlight are drawn from a wide assortment of sub-fields of physics that feed into and, indeed, are essential to our modern understanding of astrophysical systems, including: classical mechanics, fluid dynamics, thermodynamics & statistical mechanics, quantum mechanics, radiation transport, and relativity. Each time one of these equations appears in our discussion, it will be marked as a key equation so that, from the information contained in our [http://www.vistrails.org/index.php/User:Tohline/Appendix/Equation_templates key equations appendix], the reader can be guided to parallel discussions of related concepts as they have been in the above-identified, ~~notable historic~~ texts.		The key equations that we have chosen to highlight are drawn from a wide assortment of sub-fields of physics that feed into and, indeed, are essential to our modern understanding of astrophysical systems, including: classical mechanics, fluid dynamics, thermodynamics & statistical mechanics, quantum mechanics, radiation transport, and relativity. Each time one of these equations appears in our discussion, it will be marked as a key equation so that, from the information contained in our [http://www.vistrails.org/index.php/User:Tohline/Appendix/Equation_templates key equations appendix], the reader can be guided to parallel discussions of related concepts as they have been presented in the above-identified, published texts.

	It is important to note as well that virtually all of these key equations — and discussions of the physical concepts that underpin them — can also now be found in the pages of [http://www.wikipedia.org/ Wikipedia], or other online references. Where appropriate, links to these online discussions are also provided in the text of this H_Book so that readers can take advantage of this growing information resource.		It is important to note as well that virtually all of these key equations — and discussions of the physical concepts that underpin them — can also now be found in the pages of [http://www.wikipedia.org/ Wikipedia], or other online references. Where appropriate, links to these online discussions are also provided in the text of this H_Book so that readers can take advantage of this growing information resource.

Tohline: /* Preface */ fix links to Equation_templates

2010-01-25T21:45:21Z

Preface: fix links to Equation_templates

← Older revision		Revision as of 21:45, 25 January 2010
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	<i>January 24, 2010</i>		<i>January 24, 2010</i>

	In an effort to show the considerable overlap that exists between the discussions presented in this H_Book and the discussions that have appeared previously in the traditional print medium, we have constructed an [http://www.vistrails.org/index.php/User:Tohline/Appendix/~~Variables_templates~~ appendix containing a set of key physical equations] and, next to each equation, we have identified where this equation first appears in each of five different published texts. The texts that we have selected are:		In an effort to show the considerable overlap that exists between the discussions presented in this H_Book and the discussions that have appeared previously in the traditional print medium, we have constructed an [http://www.vistrails.org/index.php/User:Tohline/Appendix/Equation_templates appendix containing a set of key physical equations] and, next to each equation, we have identified where this equation first appears in each of five different published texts. The texts that we have selected are:
	# Chandrasekhar, S. (1967; originally 1939), An Introduction to the Study of Stellar Structure (Dover, New York; originally University of Chicago Press, Chicago)		# Chandrasekhar, S. (1967; originally 1939), An Introduction to the Study of Stellar Structure (Dover, New York; originally University of Chicago Press, Chicago)
	# Landau & Lifschitz		# Landau & Lifschitz
	# Kippenhahn, R. & Weigert, A. (1994), Stellar Structure and Evolution (Springer-Verlag, New York)		# Kippenhahn, R. & Weigert, A. (1994), Stellar Structure and Evolution (Springer-Verlag, New York)
	# Binney, J. & Tremaine, S. (1989), Stellar Dynamics (Princeton University Press, Princeton)		# Binney, J. & Tremaine, S. (1989), Stellar Dynamics (Princeton University Press, Princeton)
	The key equations that we have chosen to highlight are drawn from a wide assortment of sub-fields of physics that feed into and, indeed, are essential to our modern understanding of astrophysical systems, including: classical mechanics, fluid dynamics, thermodynamics & statistical mechanics, quantum mechanics, radiation transport, and relativity. Each time one of these equations appears in our discussion, it will be marked as a key equation so that, from the information contained in our [http://www.vistrails.org/index.php/User:Tohline/Appendix/~~Variables_templates~~ key equations appendix], the reader can be guided to parallel discussions of related concepts as they have been in the above-identified, notable historic texts.		The key equations that we have chosen to highlight are drawn from a wide assortment of sub-fields of physics that feed into and, indeed, are essential to our modern understanding of astrophysical systems, including: classical mechanics, fluid dynamics, thermodynamics & statistical mechanics, quantum mechanics, radiation transport, and relativity. Each time one of these equations appears in our discussion, it will be marked as a key equation so that, from the information contained in our [http://www.vistrails.org/index.php/User:Tohline/Appendix/Equation_templates key equations appendix], the reader can be guided to parallel discussions of related concepts as they have been in the above-identified, notable historic texts.

	It is important to note as well that virtually all of these key equations — and discussions of the physical concepts that underpin them — can also now be found in the pages of [http://www.wikipedia.org/ Wikipedia], or other online references. Where appropriate, links to these online discussions are also provided in the text of this H_Book so that readers can take advantage of this growing information resource.		It is important to note as well that virtually all of these key equations — and discussions of the physical concepts that underpin them — can also now be found in the pages of [http://www.wikipedia.org/ Wikipedia], or other online references. Where appropriate, links to these online discussions are also provided in the text of this H_Book so that readers can take advantage of this growing information resource.

Tohline: /* Preface */ add link to "Wikipedia"

2010-01-24T17:35:44Z

Preface: add link to "Wikipedia"

← Older revision		Revision as of 17:35, 24 January 2010
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	The key equations that we have chosen to highlight are drawn from a wide assortment of sub-fields of physics that feed into and, indeed, are essential to our modern understanding of astrophysical systems, including: classical mechanics, fluid dynamics, thermodynamics & statistical mechanics, quantum mechanics, radiation transport, and relativity. Each time one of these equations appears in our discussion, it will be marked as a key equation so that, from the information contained in our [http://www.vistrails.org/index.php/User:Tohline/Appendix/Variables_templates key equations appendix], the reader can be guided to parallel discussions of related concepts as they have been in the above-identified, notable historic texts.		The key equations that we have chosen to highlight are drawn from a wide assortment of sub-fields of physics that feed into and, indeed, are essential to our modern understanding of astrophysical systems, including: classical mechanics, fluid dynamics, thermodynamics & statistical mechanics, quantum mechanics, radiation transport, and relativity. Each time one of these equations appears in our discussion, it will be marked as a key equation so that, from the information contained in our [http://www.vistrails.org/index.php/User:Tohline/Appendix/Variables_templates key equations appendix], the reader can be guided to parallel discussions of related concepts as they have been in the above-identified, notable historic texts.

	It is important to note as well that virtually all of these key equations — and discussions of the physical concepts that underpin them — can also now be found in the pages of Wikipedia, or other online references. Where appropriate, links to these online discussions are also provided in the text of this H_Book so that readers can take advantage of this growing information resource.		It is important to note as well that virtually all of these key equations — and discussions of the physical concepts that underpin them — can also now be found in the pages of [http://www.wikipedia.org/ Wikipedia], or other online references. Where appropriate, links to these online discussions are also provided in the text of this H_Book so that readers can take advantage of this growing information resource.


	{{LSU_HBook_footer}}		{{LSU_HBook_footer}}

Tohline: /* Preface */ Improve text of January 2010 preface

2010-01-24T17:32:29Z

Preface: Improve text of January 2010 preface

← Older revision		Revision as of 17:32, 24 January 2010
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	The key equations that we have chosen to highlight are drawn from a wide assortment of sub-fields of physics that feed into and, indeed, are essential to our modern understanding of astrophysical systems, including: classical mechanics, fluid dynamics, thermodynamics & statistical mechanics, quantum mechanics, radiation transport, and relativity. Each time one of these equations appears in our discussion, it will be marked as a key equation so that, from the information contained in our [http://www.vistrails.org/index.php/User:Tohline/Appendix/Variables_templates key equations appendix], the reader can be guided to parallel discussions of related concepts as they have been in the above-identified, notable historic texts.		The key equations that we have chosen to highlight are drawn from a wide assortment of sub-fields of physics that feed into and, indeed, are essential to our modern understanding of astrophysical systems, including: classical mechanics, fluid dynamics, thermodynamics & statistical mechanics, quantum mechanics, radiation transport, and relativity. Each time one of these equations appears in our discussion, it will be marked as a key equation so that, from the information contained in our [http://www.vistrails.org/index.php/User:Tohline/Appendix/Variables_templates key equations appendix], the reader can be guided to parallel discussions of related concepts as they have been in the above-identified, notable historic texts.

	It is important to note as well that these key equations, and discussions of the physical concepts that underpin them, can now be found in the pages of Wikipedia. Where appropriate, ~~we are including~~ links to ~~key Wikipedia~~ discussions in the text of this H_Book.		It is important to note as well that virtually all of these key equations — and discussions of the physical concepts that underpin them — can also now be found in the pages of Wikipedia, or other online references. Where appropriate, links to these online discussions are also provided in the text of this H_Book so that readers can take advantage of this growing information resource.


	{{LSU_HBook_footer}}		{{LSU_HBook_footer}}

Tohline: Add 24 January 2010 preface

2010-01-24T17:21:59Z

Add 24 January 2010 preface

← Older revision		Revision as of 17:21, 24 January 2010
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	<i>November 18, 1994</i>		<i>November 18, 1994</i>

	Much of our present, basic understanding of ~~thestructure~~, stability, and dynamical evolution of individual stars,		Much of our present, basic understanding of the structure, stability, and dynamical evolution of individual stars, short-period binary star systems, and the gaseous disks that are associated with numerous types of stellar systems (including galaxies) is derived from an examination of the behavior of a specific set of coupled, partial differential equations. These equations — most of which also are heavily utilized in studies of continuum flows in terrestrial environments — are thought to govern the underlying physics of all macroscopic "fluid" systems in astronomy. Although relatively simple in form, they prove to be very rich in nature.
	short-period binary star systems, and the gaseous disks that are associated with numerous types of stellar systems (including galaxies) is derived from an examination of the behavior of a specific set of coupled, partial differential equations. These equations — most of which also are heavily utilized in studies of continuum flows in terrestrial environments — are thought to govern the underlying physics of all macroscopic "fluid" systems in
	astronomy. Although relatively simple in form, they prove to be very rich in nature.

	The literature on this subject is enormous, as serious discussions of		The literature on this subject is enormous, as serious discussions of
Line 24:		Line 22:
	*To take advantage of the added dimensions offered by the hypertext medium — such as color, text/equation linkages, animation, VRML, and access to online computational algorithms — to effectively illustrate many of these physical principles.		*To take advantage of the added dimensions offered by the hypertext medium — such as color, text/equation linkages, animation, VRML, and access to online computational algorithms — to effectively illustrate many of these physical principles.


			------


			<i>January 24, 2010</i>

			In an effort to show the considerable overlap that exists between the discussions presented in this H_Book and the discussions that have appeared previously in the traditional print medium, we have constructed an [http://www.vistrails.org/index.php/User:Tohline/Appendix/Variables_templates appendix containing a set of key physical equations] and, next to each equation, we have identified where this equation first appears in each of five different published texts. The texts that we have selected are:
			# Chandrasekhar, S. (1967; originally 1939), An Introduction to the Study of Stellar Structure (Dover, New York; originally University of Chicago Press, Chicago)
			# Landau & Lifschitz
			# Kippenhahn, R. & Weigert, A. (1994), Stellar Structure and Evolution (Springer-Verlag, New York)
			# Binney, J. & Tremaine, S. (1989), Stellar Dynamics (Princeton University Press, Princeton)
			The key equations that we have chosen to highlight are drawn from a wide assortment of sub-fields of physics that feed into and, indeed, are essential to our modern understanding of astrophysical systems, including: classical mechanics, fluid dynamics, thermodynamics & statistical mechanics, quantum mechanics, radiation transport, and relativity. Each time one of these equations appears in our discussion, it will be marked as a key equation so that, from the information contained in our [http://www.vistrails.org/index.php/User:Tohline/Appendix/Variables_templates key equations appendix], the reader can be guided to parallel discussions of related concepts as they have been in the above-identified, notable historic texts.

			It is important to note as well that these key equations, and discussions of the physical concepts that underpin them, can now be found in the pages of Wikipedia. Where appropriate, we are including links to key Wikipedia discussions in the text of this H_Book.

	{{LSU_HBook_footer}}		{{LSU_HBook_footer}}

Tohline: inserted header and footer

2010-01-20T04:44:24Z

inserted header and footer

← Older revision		Revision as of 04:44, 20 January 2010
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	__NOTOC__		__NOTOC__

	~~[[Image:H_Book_title.gif\|550px\|center]]~~		{{LSU_HBook_header}}

	==Preface==		==Preface==
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	*To take advantage of the added dimensions offered by the hypertext medium — such as color, text/equation linkages, animation, VRML, and access to online computational algorithms — to effectively illustrate many of these physical principles.		*To take advantage of the added dimensions offered by the hypertext medium — such as color, text/equation linkages, animation, VRML, and access to online computational algorithms — to effectively illustrate many of these physical principles.

	~~----~~

	~~<div align="center">~~		{{LSU_HBook_footer}}
	~~[http://www.vistrails.org/index.php/User:Tohline/H_Book Home] \|~~
	~~</div>~~

Tohline: /* Preface */ insert em dash

2010-01-20T04:41:51Z

Preface: insert em dash

← Older revision		Revision as of 04:41, 20 January 2010
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	Much of our present, basic understanding of thestructure, stability, and dynamical evolution of individual stars,		Much of our present, basic understanding of thestructure, stability, and dynamical evolution of individual stars,
	short-period binary star systems, and the gaseous disks that are associated with numerous types of stellar systems (including galaxies) is derived from an examination of the behavior of a specific set of coupled, partial differential equations. These equations &#~~150~~; most of which also are heavily utilized in studies of continuum flows in terrestrial environments &#~~150~~; are thought to govern the underlying physics of all macroscopic "fluid" systems in		short-period binary star systems, and the gaseous disks that are associated with numerous types of stellar systems (including galaxies) is derived from an examination of the behavior of a specific set of coupled, partial differential equations. These equations — most of which also are heavily utilized in studies of continuum flows in terrestrial environments — are thought to govern the underlying physics of all macroscopic "fluid" systems in
	astronomy. Although relatively simple in form, they prove to be very rich in nature.		astronomy. Although relatively simple in form, they prove to be very rich in nature.

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	*To document in an electronically accessible format many of the key physical principles that underlie modern discussions of the structure, stability, and dynamical evolution of astrophysical fluid systems;		*To document in an electronically accessible format many of the key physical principles that underlie modern discussions of the structure, stability, and dynamical evolution of astrophysical fluid systems;

	*To take advantage of the added dimensions offered by the hypertext medium &#~~150~~; such as color, text/equation linkages, animation, VRML, and access to online computational algorithms &#~~150~~; to effectively illustrate many of these physical principles.		*To take advantage of the added dimensions offered by the hypertext medium — such as color, text/equation linkages, animation, VRML, and access to online computational algorithms — to effectively illustrate many of these physical principles.

	----		----

Tohline: /* Preface */ insert correct character entity for hyphen (Em dash)

2010-01-18T18:18:31Z

Preface: insert correct character entity for hyphen (Em dash)

← Older revision		Revision as of 18:18, 18 January 2010
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	<i>November 18, 1994</i>		<i>November 18, 1994</i>

	Much of our present, basic understanding of ~~the~~		Much of our present, basic understanding of thestructure, stability, and dynamical evolution of individual stars,
	~~structure~~, stability, and dynamical evolution of individual stars,		short-period binary star systems, and the gaseous disks that are associated with numerous types of stellar systems (including galaxies) is derived from an examination of the behavior of a specific set of coupled, partial differential equations. These equations most of which also are heavily utilized in studies of continuum flows in terrestrial environments are thought to govern the underlying physics of all macroscopic "fluid" systems in
	short-period binary star systems, and the gaseous disks that are associated		astronomy. Although relatively simple in form, they prove to be very rich in nature.
	with numerous types of stellar systems (including galaxies) is derived
	from an examination of the behavior of a specific set of coupled, partial differential equations. These equations -- most of which also are heavily utilized in studies of continuum flows in terrestrial environments -- are thought to
	govern the underlying physics of all macroscopic "fluid" systems in
	astronomy. Although relatively simple in form, they prove to be very rich
	in nature.

	The literature on this subject is enormous, as serious discussions of		The literature on this subject is enormous, as serious discussions of
Line 27:		Line 22:
	*To document in an electronically accessible format many of the key physical principles that underlie modern discussions of the structure, stability, and dynamical evolution of astrophysical fluid systems;		*To document in an electronically accessible format many of the key physical principles that underlie modern discussions of the structure, stability, and dynamical evolution of astrophysical fluid systems;

	*To take advantage of the added dimensions offered by the hypertext medium -- such as color, text/equation linkages, animation, VRML, and access to online computational algorithms -- to effectively illustrate many of these physical principles.		*To take advantage of the added dimensions offered by the hypertext medium such as color, text/equation linkages, animation, VRML, and access to online computational algorithms to effectively illustrate many of these physical principles.

	----		----