OldVistrailsCoverPage - Revision history

Jet53man: /* Useful Links */

2022-04-20T23:42:24Z

Useful Links

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	** To set a redirect: #REDIRECT [[User:Tohline/page]]		** To set a redirect: #REDIRECT [[User:Tohline/page]]
	** To set internal link: [[User:Tohline/page \| text]]		** To set internal link: [[User:Tohline/page \| text]]
	*[http://en.wikipedia.org/wiki/Help:Wiki_markup Wiki Markup]; [https://www.mediawiki.org/wiki/Help:Tables#With_HTML_attributes_and_CSS_styles MediaWiki CSS Style Sheet] and [[~~User:Tohline/~~SSC/~~Synopsis_StyleSheet~~\|Example]]		*[http://en.wikipedia.org/wiki/Help:Wiki_markup Wiki Markup]; [https://www.mediawiki.org/wiki/Help:Tables#With_HTML_attributes_and_CSS_styles MediaWiki CSS Style Sheet] and [[SSC/SynopsisStyleSheet\|Example]]
	*[https://meta.wikimedia.org/wiki/Help:Displaying_a_formula LaTeX examples]; [ftp://sunsite.icm.edu.pl/pub/CTAN/info/symbols/comprehensive/symbols-a4.pdf A comprehensive LaTeX symbol list]		*[https://meta.wikimedia.org/wiki/Help:Displaying_a_formula LaTeX examples]; [ftp://sunsite.icm.edu.pl/pub/CTAN/info/symbols/comprehensive/symbols-a4.pdf A comprehensive LaTeX symbol list]
	*[http://en.wikipedia.org/wiki/Character_entities Character Entities]; [http://www.alanwood.net/demos/ent4_frame.html HTML Character Entities]; [http://www.johndcook.com/blog/math_symbols/ MathSymbols]		*[http://en.wikipedia.org/wiki/Character_entities Character Entities]; [http://www.alanwood.net/demos/ent4_frame.html HTML Character Entities]; [http://www.johndcook.com/blog/math_symbols/ MathSymbols]

Jet53man: /* Challenges to Young, Applied Mathematicians */

2022-04-20T23:40:53Z

Challenges to Young, Applied Mathematicians

← Older revision		Revision as of 19:40, 20 April 2022
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	<font color="red">'''Note from J. E. Tohline to Students with Good Mathematical Skills'''</font>: The astronomy community's understanding of the ''Structure, Stability, and Dynamics'' of stars and galaxies would be strengthened if we had, in hand, closed-form analytic solutions to the following well-defined mathematical problems. (Solutions can be obtained ''numerically'' with relative ease, but here the challenge is to find a closed-form analytic solution.) As is true with most meaningful scientific research projects, it is not at all clear whether each of these problems ''has'' a solution. In my judgment, however, it seems plausible that a closed-form solution can be discovered in each case and such a solution would be of sufficient interest to the astronomical community that it would likely be publishable in a professional astronomy or physics journal. At the very least, each of these projects represents an opportunity for a graduate student, an undergraduate, or even a talented high-school student (perhaps in connection with a mathematics science fair project?) to hone her/his research skills in applied mathematics. Also, I would be thrilled to include a solution to any one of these problems — along with full credit to the solution's author — as a chapter in this online H_Book. Having retired from LSU, I am not in a position to financially support or formally advise students who are in pursuit of a higher-education degree. I would nevertheless be interested in sharing my expertise — and, perhaps, developing a collaborative relationship — with individuals who are interested in pursuing answers to the questions posed by this identified set of problems.		<font color="red">'''Note from J. E. Tohline to Students with Good Mathematical Skills'''</font>: The astronomy community's understanding of the ''Structure, Stability, and Dynamics'' of stars and galaxies would be strengthened if we had, in hand, closed-form analytic solutions to the following well-defined mathematical problems. (Solutions can be obtained ''numerically'' with relative ease, but here the challenge is to find a closed-form analytic solution.) As is true with most meaningful scientific research projects, it is not at all clear whether each of these problems ''has'' a solution. In my judgment, however, it seems plausible that a closed-form solution can be discovered in each case and such a solution would be of sufficient interest to the astronomical community that it would likely be publishable in a professional astronomy or physics journal. At the very least, each of these projects represents an opportunity for a graduate student, an undergraduate, or even a talented high-school student (perhaps in connection with a mathematics science fair project?) to hone her/his research skills in applied mathematics. Also, I would be thrilled to include a solution to any one of these problems — along with full credit to the solution's author — as a chapter in this online H_Book. Having retired from LSU, I am not in a position to financially support or formally advise students who are in pursuit of a higher-education degree. I would nevertheless be interested in sharing my expertise — and, perhaps, developing a collaborative relationship — with individuals who are interested in pursuing answers to the questions posed by this identified set of problems.

	* [[~~User:Tohline/~~MathProjects/EigenvalueProblemN1\|Find Analytic Solutions to an Eigenvalue Problem]]		* [[MathProjects/EigenvalueProblemN1\|Find Analytic Solutions to an Eigenvalue Problem]]



	~~{{LSU_HorizontalLine}}~~

	== Useful Links ==		== Useful Links ==

Jet53man: /* Gravitational-Wave Signals from Core-Collapse Supernovae */

2022-04-20T23:38:02Z

Gravitational-Wave Signals from Core-Collapse Supernovae

← Older revision		Revision as of 19:38, 20 April 2022
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	===Gravitational-Wave Signals from Core-Collapse Supernovae===		===Gravitational-Wave Signals from Core-Collapse Supernovae===
	To date, gravitational radiation has not been directly detected by any scientific instrument on Earth. The advancement of detector techniques in association with the development of new observatories worldwide — such as [http://www.ligo.org/ LIGO] and [http://wwwcascina.virgo.infn.it/ VIRGO] — promises to change this situation in the near future. When gravitational-wave signals are detected from core-collapse supernovae, the expectation is that these signals — primarily tracing out wave amplitude as a function of time — will exhibit a great deal of structure, reflecting several different phases of the collapse. We propose to construct a semi-analytic signal template to help the gravitational-wave community more fully understand the underlying physics that is fundamentally responsible for generating the (anticipated) signal's characteristic features.		To date, gravitational radiation has not been directly detected by any scientific instrument on Earth. The advancement of detector techniques in association with the development of new observatories worldwide — such as [http://www.ligo.org/ LIGO] and [http://wwwcascina.virgo.infn.it/ VIRGO] — promises to change this situation in the near future. When gravitational-wave signals are detected from core-collapse supernovae, the expectation is that these signals — primarily tracing out wave amplitude as a function of time — will exhibit a great deal of structure, reflecting several different phases of the collapse. We propose to construct a semi-analytic signal template to help the gravitational-wave community more fully understand the underlying physics that is fundamentally responsible for generating the (anticipated) signal's characteristic features.
	* [[ProjectsUnderway/~~Core_Collapse_Supernovae~~#A_Template_for_Gravitational_Wave_Signals_from_Core-Collapse_Supernovae\|A Template for Gravitational-Wave Signals from Core-Collapse Supernovae]]		* [[ProjectsUnderway/CoreCollapseSupernovae#A_Template_for_Gravitational_Wave_Signals_from_Core-Collapse_Supernovae\|A Template for Gravitational-Wave Signals from Core-Collapse Supernovae]]
	* Relevant to …		* Relevant to …

Jet53man: /* Stability of Bipolytropic Configurations */

2022-04-20T23:37:23Z

Stability of Bipolytropic Configurations

← Older revision		Revision as of 19:37, 20 April 2022
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	<td align="left">[[SSC/Structure/LimitingMasses#Bounded_Isothermal_Sphere_.26_Bonnor-Ebert_Mass\|Bonnor-Ebert Spheres]]</td></tr>		<td align="left">[[SSC/Structure/LimitingMasses#Bounded_Isothermal_Sphere_.26_Bonnor-Ebert_Mass\|Bonnor-Ebert Spheres]]</td></tr>
	<tr><td width="4%" align="left">   </td>		<tr><td width="4%" align="left">   </td>
	<td align="left">Origin of Planetary Nebulae</td></tr>		<td align="left">[[Appendix/Ramblings/OriginOfPlanetaryNebulae\|Origin of Planetary Nebulae]]</td></tr>
	</table>		</table>

Jet53man: /* Globular Cluster Formation During Galaxy-Galaxy Collisions */

2022-04-20T23:14:45Z

Globular Cluster Formation During Galaxy-Galaxy Collisions

← Older revision		Revision as of 19:14, 20 April 2022
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	* Original manuscript (submitted to ''The Astrophysical Journal'' in June, 2000): [http://www.vistrails.org/images/Ms_globularClusters.pdf J. E. Tohline, N. Z. Scoville, & A. W. Strong (2000)]		* Original manuscript (submitted to ''The Astrophysical Journal'' in June, 2000): [http://www.vistrails.org/images/Ms_globularClusters.pdf J. E. Tohline, N. Z. Scoville, & A. W. Strong (2000)]

	This paper was never published because the journal referee (see [[~~User:Tohline/~~DissertationTopics/GCFormation#RefereeReport\|accompanying material]]) requested a more extensive demonstration of the proposed model's viability, which I considered to be well beyond the scope and essential purpose of this paper. I remain firmly convinced that the idea has a great deal of merit. I offer this original manuscript as a foundation on which an appropriately qualified graduate student might build a more extensive demonstration of the viability of this proposed mechanism for globular cluster formation.		This paper was never published because the journal referee (see [[DissertationTopics/GCFormation#RefereeReport\|accompanying material]]) requested a more extensive demonstration of the proposed model's viability, which I considered to be well beyond the scope and essential purpose of this paper. I remain firmly convinced that the idea has a great deal of merit. I offer this original manuscript as a foundation on which an appropriately qualified graduate student might build a more extensive demonstration of the viability of this proposed mechanism for globular cluster formation.

	==Other Less Challenging or Less Well-Defined Research Projects==		==Other Less Challenging or Less Well-Defined Research Projects==

Jet53man: /* Other Less Challenging or Less Well-Defined Research Projects */

2022-04-20T00:11:39Z

Other Less Challenging or Less Well-Defined Research Projects

← Older revision		Revision as of 20:11, 19 April 2022
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	===Stability of Bipolytropic Configurations===		===Stability of Bipolytropic Configurations===
	Using primarily analytic techniques, our objective is to evaluate the free energy of spherically symmetric, bipolytropic configurations (''aka'' composite polytropes), then, use variations in the free energy function to identify equilibrium states (scalar virial theorem) and to assess the relative dynamical stability of the states.		Using primarily analytic techniques, our objective is to evaluate the free energy of spherically symmetric, bipolytropic configurations (''aka'' composite polytropes), then, use variations in the free energy function to identify equilibrium states (scalar virial theorem) and to assess the relative dynamical stability of the states.
	* Early discussions with LSU graduate student, [[~~User:Tohline/~~SSC/VirialStability#Discussion_with_Kundan_Kadam\|Kundan Kadam]]; see also [[~~User:Tohline/~~SSC/Structure/BiPolytropes/~~Analytic0_0~~#BiPolytrope_with_nc_.3D_0_and_ne_.3D_0\|construction of <math>~(n_c, n_e) = (0, 0)</math> bipolytrope]]		* Early discussions with LSU graduate student, [[SSC/VirialStability#Discussion_with_Kundan_Kadam\|Kundan Kadam]]; see also [[SSC/Structure/BiPolytropes/Analytic00#BiPolytrope_with_nc_.3D_0_and_ne_.3D_0\|construction of <math>(n_c, n_e) = (0, 0)</math> bipolytrope]]
	* Outline of [[~~User:Tohline/~~SSC/Virial/PolytropesEmbeddedOutline#Outline\|Work Completed, to Date]], on the free energy of pressure-truncated polytropes		* Outline of [[SSC/Virial/PolytropesEmbeddedOutline#Outline\|Work Completed, to Date]], on the free energy of pressure-truncated polytropes
	* Relevant to …		* Relevant to …
	~~<div>~~
	<table border="0" cellpadding="1" align="~~left~~" width="100%">		<table border="0" cellpadding="1" align="center" width="100%">
	<tr><td width="4%" align="left">   </td>		<tr><td width="4%" align="left">   </td>
	<td align="left">[[~~User:Tohline/~~SSC/Structure/LimitingMasses#Sch.C3.B6nberg-Chandrasekhar_Mass\|Schönberg-Chandrasekhar Mass]]</td></tr>		<td align="left">[[SSC/Structure/LimitingMasses#Sch.C3.B6nberg-Chandrasekhar_Mass\|Schönberg-Chandrasekhar Mass]]</td></tr>
	<tr><td width="4%" align="left">   </td>		<tr><td width="4%" align="left">   </td>
	<td align="left">[[~~User:Tohline/~~SSC/Structure/BiPolytropes/~~Analytic5_1~~#Derivation_by_Eggleton.2C_Faulkner.2C_and_Cannon_.281998.29\|Stellar Evolution from Main Sequence to Red Giant]]</td></tr>		<td align="left">[[SSC/Structure/BiPolytropes/Analytic51#Derivation_by_Eggleton.2C_Faulkner.2C_and_Cannon_.281998.29\|Stellar Evolution from Main Sequence to Red Giant]]</td></tr>
	<tr><td width="4%" align="left">   </td>		<tr><td width="4%" align="left">   </td>
	<td align="left">[[~~User:Tohline/~~SSC/Structure/LimitingMasses#Bounded_Isothermal_Sphere_.26_Bonnor-Ebert_Mass\|Bonnor-Ebert Spheres]]</td></tr>		<td align="left">[[SSC/Structure/LimitingMasses#Bounded_Isothermal_Sphere_.26_Bonnor-Ebert_Mass\|Bonnor-Ebert Spheres]]</td></tr>
	<tr><td width="4%" align="left">   </td>		<tr><td width="4%" align="left">   </td>
	<td align="left">Origin of Planetary Nebulae</td></tr>		<td align="left">Origin of Planetary Nebulae</td></tr>
	~~<tr><td colspan="2"> </td></tr>~~
	</table>		</table>
	~~</div>~~

	===Gravitational-Wave Signals from Core-Collapse Supernovae===		===Gravitational-Wave Signals from Core-Collapse Supernovae===
	To date, gravitational radiation has not been directly detected by any scientific instrument on Earth. The advancement of detector techniques in association with the development of new observatories worldwide — such as [http://www.ligo.org/ LIGO] and [http://wwwcascina.virgo.infn.it/ VIRGO] — promises to change this situation in the near future. When gravitational-wave signals are detected from core-collapse supernovae, the expectation is that these signals — primarily tracing out wave amplitude as a function of time — will exhibit a great deal of structure, reflecting several different phases of the collapse. We propose to construct a semi-analytic signal template to help the gravitational-wave community more fully understand the underlying physics that is fundamentally responsible for generating the (anticipated) signal's characteristic features.		To date, gravitational radiation has not been directly detected by any scientific instrument on Earth. The advancement of detector techniques in association with the development of new observatories worldwide — such as [http://www.ligo.org/ LIGO] and [http://wwwcascina.virgo.infn.it/ VIRGO] — promises to change this situation in the near future. When gravitational-wave signals are detected from core-collapse supernovae, the expectation is that these signals — primarily tracing out wave amplitude as a function of time — will exhibit a great deal of structure, reflecting several different phases of the collapse. We propose to construct a semi-analytic signal template to help the gravitational-wave community more fully understand the underlying physics that is fundamentally responsible for generating the (anticipated) signal's characteristic features.
	* [[~~User:Tohline/~~ProjectsUnderway/Core_Collapse_Supernovae#A_Template_for_Gravitational_Wave_Signals_from_Core-Collapse_Supernovae\|A Template for Gravitational-Wave Signals from Core-Collapse Supernovae]]		* [[ProjectsUnderway/Core_Collapse_Supernovae#A_Template_for_Gravitational_Wave_Signals_from_Core-Collapse_Supernovae\|A Template for Gravitational-Wave Signals from Core-Collapse Supernovae]]
	* Relevant to …		* Relevant to …
	~~<div>~~
	<table border="0" cellpadding="1" align="~~left~~" width="100%">		<table border="0" cellpadding="1" align="center" width="100%">
	<tr><td width="4%" align="left">   </td>		<tr><td width="4%" align="left">   </td>
	<td align="left">[[~~User:Tohline~~/~~SSC~~/FreeFall#Free-Fall_Collapse\|Gravitational Free-Fall Collapse]]</td></tr>		<td align="left">[[SSC/Dynamics/FreeFall#Free-Fall_Collapse\|Gravitational Free-Fall Collapse]]</td></tr>
	<tr><td width="4%" align="left">   </td>		<tr><td width="4%" align="left">   </td>
	<td align="left">[[~~User:Tohline/~~Apps/GoldreichWeber80#Homologously_Collapsing_Stellar_Cores\|Homologous Collapse of Stellar Cores]] (Goldreich & Weber 1980)~~</td></tr>~~		<td align="left">[[Apps/GoldreichWeber80#Homologously_Collapsing_Stellar_Cores\|Homologous Collapse of Stellar Cores]] (Goldreich & Weber 1980)</td></tr>
	~~<tr><td colspan="2"> ~~</td></tr>
	</table>		</table>
	~~</div>~~

	===Musings Regarding Dark Matter and Dark Energy===		===Musings Regarding Dark Matter and Dark Energy===
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	* [http://www.phys.lsu.edu/~tohline/TinsleyNotes1978.pdf Notes from Beatrice Tinsley] showing that she, too, had given some thought to the implications of a 1/r force-law for gravity in 1978.		* [http://www.phys.lsu.edu/~tohline/TinsleyNotes1978.pdf Notes from Beatrice Tinsley] showing that she, too, had given some thought to the implications of a 1/r force-law for gravity in 1978.

	* [[~~User:Tohline/~~DarkMatter/VeraRubin\|Early interactions with Vera Rubin]].		* [[DarkMatter/VeraRubin\|Early interactions with Vera Rubin]].

	* [[User:Tohline/DarkMatter/UniformSphere\|Attraction associated with a uniform-density sphere]] — my derivation in the early '80s, with the kind assistance of LSU Professor Attipat K. Rajagopal.

	* [[User:Tohline/DarkMatter/CK2015\|Remarks on Christodoulou & Kazanas (2015)]]

	* [[~~User:Tohline~~/~~Appendix/Ramblings/StrongNuclearForce~~\|~~Radial Dependence of the Strong Nuclear Force~~]]		* [[DarkMatter/UniformSphere\|Attraction associated with a uniform-density sphere]] — my derivation in the early '80s, with the kind assistance of LSU Professor Attipat K. Rajagopal.

			* [[DarkMatter/CK2015\|Remarks on Christodoulou & Kazanas (2015)]]

	~~{{LSU_HorizontalLine}}~~		* [[Appendix/Ramblings/StrongNuclearForce\|Radial Dependence of the Strong Nuclear Force]]

	==Challenges to Young, Applied Mathematicians==		==Challenges to Young, Applied Mathematicians==

Jet53man: /* Suggested Doctoral Dissertation-Level Research Projects */

2022-04-20T00:04:19Z

Suggested Doctoral Dissertation-Level Research Projects

← Older revision		Revision as of 20:04, 19 April 2022
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	* Relevant to …		* Relevant to …

	<table border="1" cellpadding="1" align="~~left~~" width="100%">		<table border="0" cellpadding="1" align="center" width="100%">
	<tr>		<tr>
	<td width="4%" align="left">   </td>		<td width="4%" align="left">   </td>

Jet53man: /* Suggested Doctoral Dissertation-Level Research Projects */

2022-04-20T00:03:11Z

Suggested Doctoral Dissertation-Level Research Projects

← Older revision		Revision as of 20:03, 19 April 2022
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	===Globular Cluster Formation During Galaxy-Galaxy Collisions===		===Globular Cluster Formation During Galaxy-Galaxy Collisions===

	The manuscript presented immediately below presents an hypothesis regarding globular cluster formation that came to me as a EUREKA! moment one day (in the mid-to-late 1990s) while I was attending a Physics & Astronomy departmental colloquium at LSU. The colloquium speaker was, as I recall, someone from U. C. Berkeley with experimental space sciences expertise; and the topic of the colloquium was Galactic cosmic rays … [[DissertationTopics/GCFormation\|<more>]]		The manuscript presented immediately below presents an hypothesis regarding globular cluster formation that came to me as a EUREKA! moment one day (in the mid-to-late 1990s) while I was attending a Physics & Astronomy departmental colloquium at LSU. The colloquium speaker was, as I recall, someone from U. C. Berkeley with experimental space sciences expertise; and the topic of the colloquium was Galactic cosmic rays … [[DissertationTopics/GCFormation\|<more>]]

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	This paper was never published because the journal referee (see [[User:Tohline/DissertationTopics/GCFormation#RefereeReport\|accompanying material]]) requested a more extensive demonstration of the proposed model's viability, which I considered to be well beyond the scope and essential purpose of this paper. I remain firmly convinced that the idea has a great deal of merit. I offer this original manuscript as a foundation on which an appropriately qualified graduate student might build a more extensive demonstration of the viability of this proposed mechanism for globular cluster formation.		This paper was never published because the journal referee (see [[User:Tohline/DissertationTopics/GCFormation#RefereeReport\|accompanying material]]) requested a more extensive demonstration of the proposed model's viability, which I considered to be well beyond the scope and essential purpose of this paper. I remain firmly convinced that the idea has a great deal of merit. I offer this original manuscript as a foundation on which an appropriately qualified graduate student might build a more extensive demonstration of the viability of this proposed mechanism for globular cluster formation.

	~~{{LSU_HorizontalLine}}~~

	==Other Less Challenging or Less Well-Defined Research Projects==		==Other Less Challenging or Less Well-Defined Research Projects==

Jet53man: /* Suggested Doctoral Dissertation-Level Research Projects */

2022-04-20T00:00:57Z

Suggested Doctoral Dissertation-Level Research Projects

← Older revision		Revision as of 20:00, 19 April 2022
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	==Suggested Doctoral Dissertation-Level Research Projects==		==Suggested Doctoral Dissertation-Level Research Projects==
	Over the years — dating back to my time as a J. Willard Gibbs Instructor at Yale University (1978 - 1980) and throughout my academic career at LSU (see [[~~User:Tohline~~/~~LSU~~/~~Students~~#~~StudentList~~\|an accompanying list]]) — I have helped more than twenty physics and/or astronomy graduate students identify a suitable topic for their doctoral dissertation research. Although, in retirement, I am no longer formally advising doctoral students, I continue to recognize dissertation-level research projects that are ripe for investigation. Here are brief descriptions of a number of such projects. As time goes along, I expect to add chapters to my [[~~User:Tohline/H_Book#Applications~~\|online H_Book]] that will supply each of these projects with a more substantive background foundation. I would be happy to hand each of these projects off to an appropriately qualified graduate student who expresses sufficient interest in tackling the project in depth.		Over the years — dating back to my time as a J. Willard Gibbs Instructor at Yale University (1978 - 1980) and throughout my academic career at LSU (see [[Appendix/Ramblings/MyDoctoralStudents#Doctoral_Students_Tohline_Has_Advised\|an accompanying list]]) — I have helped more than twenty physics and/or astronomy graduate students identify a suitable topic for their doctoral dissertation research. Although, in retirement, I am no longer formally advising doctoral students, I continue to recognize dissertation-level research projects that are ripe for investigation. Here are brief descriptions of a number of such projects. As time goes along, I expect to add chapters to my [[Main_Page\|online H_Book]] that will supply each of these projects with a more substantive background foundation. I would be happy to hand each of these projects off to an appropriately qualified graduate student who expresses sufficient interest in tackling the project in depth.

	===Constructing Compressible Analogs of Riemann Ellipsoids===		===Constructing Compressible Analogs of Riemann Ellipsoids===
	We have known, for well over 100 years, that rapidly rotating, ellipsoidal-shaped equilibrium configurations can be constructed with a variety of different internal fluid velocity profiles — giving rise to Jacobi, Dedekind, or Riemann ellipsoids — ''if the fluid configuration has uniform density and is incompressible.'' [http://adsabs.harvard.edu/abs/2000ApJ...532.1051C Computational fluid-dynamic (CFD) simulations have demonstrated] that dynamically stable compressible analogs of Riemann ellipsoids can be constructed, under certain conditions. The objective here is to develop a numerical technique, akin to the [http://www.phys.lsu.edu/astro/H_Book.current/Applications/Structure/HSCF_Code/HSCF.html Hachisu self-consistent field (HSCF) technique], by which a wide range of such equilibrium configurations can be constructed ''a priori'', without relying on CFD techniques.		We have known, for well over 100 years, that rapidly rotating, ellipsoidal-shaped equilibrium configurations can be constructed with a variety of different internal fluid velocity profiles — giving rise to Jacobi, Dedekind, or Riemann ellipsoids — ''if the fluid configuration has uniform density and is incompressible.'' [http://adsabs.harvard.edu/abs/2000ApJ...532.1051C Computational fluid-dynamic (CFD) simulations have demonstrated] that dynamically stable compressible analogs of Riemann ellipsoids can be constructed, under certain conditions. The objective here is to develop a numerical technique, akin to the [http://www.phys.lsu.edu/astro/H_Book.current/Applications/Structure/HSCF_Code/HSCF.html Hachisu self-consistent field (HSCF) technique], by which a wide range of such equilibrium configurations can be constructed ''a priori'', without relying on CFD techniques.
	* [http://adsabs.harvard.edu/abs/2006ApJ...639..549O Shangli Ou] developed an HSCF-type technique that successfully constructs ''approximate'' equilibrium configurations that are analogs of Riemann ellipsoids		* [http://adsabs.harvard.edu/abs/2006ApJ...639..549O Shangli Ou] developed an HSCF-type technique that successfully constructs ''approximate'' equilibrium configurations that are analogs of Riemann ellipsoids
	* [[~~User:Tohline/~~Apps/~~RiemannEllipsoids_Compressible~~\|Some thoughts regarding]] how a more satisfactory velocity flow-field might be incorporated into Ou's technique in order to achieve this project objective		* [[Apps/RiemannEllipsoidsCompressible\|Some thoughts regarding]] how a more satisfactory velocity flow-field might be incorporated into Ou's technique in order to achieve this project objective
	* Apart from my astronomy colleagues at LSU, I have had especially useful discussions of this project with Eric Hirschmann (BYU), David Neilsen (BYU), [https://www.semanticscholar.org/paper/A-hybrid-variational-level-set-approach-to-handle-Walker/7ee624ab9ffe45241cb0e5a0ce0898a6da201e7b Shawn W. Walker (2007)] (LSU Mathematics & CCT), and Ricardo H. Nochetto (U. Maryland, Mathematics)		* Apart from my astronomy colleagues at LSU, I have had especially useful discussions of this project with Eric Hirschmann (BYU), David Neilsen (BYU), [https://www.semanticscholar.org/paper/A-hybrid-variational-level-set-approach-to-handle-Walker/7ee624ab9ffe45241cb0e5a0ce0898a6da201e7b Shawn W. Walker (2007)] (LSU Mathematics & CCT), and Ricardo H. Nochetto (U. Maryland, Mathematics)
	* Relevant to …		* Relevant to …
	~~<div>~~
	<table border="0" cellpadding="1" align="left" width="100%">		<table border="1" cellpadding="1" align="left" width="100%">
	<tr><td width="4%" align="left">   </td>		<tr>
	<td align="left">[http://www.phys.lsu.edu/astro/movie_captions/fission.html The fission hypothesis for binary star formation]</td></tr>		<td width="4%" align="left">   </td>
	<tr><td width="4%" align="left">   </td>		<td align="left">[http://www.phys.lsu.edu/astro/movie_captions/fission.html The fission hypothesis for binary star formation]</td>
	<td align="left">[http://www.phys.lsu.edu/~tohline/fission.movies.html Fission-related CFD simulations conducted at LSU]</td></tr>		</tr>
	<tr><td width="4%" align="left">   </td>		<tr>
	<td align="left">[[~~User:Tohline/~~ThreeDimensionalConfigurations/BinaryFission#Fission_Hypothesis_of_Binary_Star_Formation\|Fission of liquid drops in spacelab experiments]]</td></tr>		<td width="4%" align="left">   </td>
	<tr><td width="4%" align="left">   </td>		<td align="left">[http://www.phys.lsu.edu/~tohline/fission.movies.html Fission-related CFD simulations conducted at LSU]</td>
	<td align="left">[http://www.phys.lsu.edu/astro/nap98/bf.final.html The Formation of Common-Envelope, Pre-Main-Sequence Binary Stars]</td~~></tr~~>		</tr>
	~~<tr><td colspan="2"> </td>~~</tr>		<tr>
			<td width="4%" align="left">   </td>
			<td align="left">[[ThreeDimensionalConfigurations/BinaryFission#Fission_Hypothesis_of_Binary_Star_Formation\|Fission of liquid drops in spacelab experiments]]</td>
			</tr>
			<tr>
			<td width="4%" align="left">   </td>
			<td align="left">[http://www.phys.lsu.edu/astro/nap98/bf.final.html The Formation of Common-Envelope, Pre-Main-Sequence Binary Stars]</td>
			</tr>
	</table>		</table>
	~~</div>~~

	===Globular Cluster Formation During Galaxy-Galaxy Collisions===		===Globular Cluster Formation During Galaxy-Galaxy Collisions===
	The manuscript presented immediately below presents an hypothesis regarding globular cluster formation that came to me as a EUREKA! moment one day (in the mid-to-late 1990s) while I was attending a Physics & Astronomy departmental colloquium at LSU. The colloquium speaker was, as I recall, someone from U. C. Berkeley with experimental space sciences expertise; and the topic of the colloquium was Galactic cosmic rays … [[~~User:Tohline/~~DissertationTopics/GCFormation\|<more>]]		The manuscript presented immediately below presents an hypothesis regarding globular cluster formation that came to me as a EUREKA! moment one day (in the mid-to-late 1990s) while I was attending a Physics & Astronomy departmental colloquium at LSU. The colloquium speaker was, as I recall, someone from U. C. Berkeley with experimental space sciences expertise; and the topic of the colloquium was Galactic cosmic rays … [[DissertationTopics/GCFormation\|<more>]]

	As a matter of course during his presentation, the colloquium speaker reminded the audience — and me, in particular — that, in our Galaxy, the dense, cold "protostellar" cores of molecular clouds are coupled to the interstellar magnetic field (only) because the gas is partially ionized by Galactic cosmic rays. Furthermore, the Galaxy's charged-particle cosmic-ray flux is highest near the mid-plane of the Galaxy's disk because the cosmic rays are trapped by the disk's relatively ordered, large-scale interstellar magnetic field. All of a sudden, it occurred to me that, if our Galaxy were to collide with another galaxy …		As a matter of course during his presentation, the colloquium speaker reminded the audience — and me, in particular — that, in our Galaxy, the dense, cold "protostellar" cores of molecular clouds are coupled to the interstellar magnetic field (only) because the gas is partially ionized by Galactic cosmic rays. Furthermore, the Galaxy's charged-particle cosmic-ray flux is highest near the mid-plane of the Galaxy's disk because the cosmic rays are trapped by the disk's relatively ordered, large-scale interstellar magnetic field. All of a sudden, it occurred to me that, if our Galaxy were to collide with another galaxy …

Jet53man: /* Joel E. Tohline */

2022-04-19T23:50:35Z

Joel E. Tohline

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	=Joel E. Tohline=		=Joel E. Tohline=
	A Fellow of the [http://www.aaas.org/ AAAS], Tohline has authored approximately one hundred articles in scientific journals and proceedings, primarily on problems related to complex fluid flows in astrophysical settings. His expertise in utilizing high-performance computers to accurately simulate the processes by which stars form and to simulate catastrophic events that will give rise to bursts of gravitational radiation is recognized worldwide. [[~~LSU~~/~~Students~~#~~StudentList~~\|Fifteen students]] have completed their doctoral dissertation research under his direction (an additional four under his co-direction) and, over the years, he has been a lead investigator on federal and state research or research-infrastructure grants totaling more than ten million dollars.		A Fellow of the [http://www.aaas.org/ AAAS], Tohline has authored approximately one hundred articles in scientific journals and proceedings, primarily on problems related to complex fluid flows in astrophysical settings. His expertise in utilizing high-performance computers to accurately simulate the processes by which stars form and to simulate catastrophic events that will give rise to bursts of gravitational radiation is recognized worldwide. [[Appendix/Ramblings/MyDoctoralStudents#Doctoral_Students_Tohline_Has_Advised\|Fifteen students]] have completed their doctoral dissertation research under his direction (an additional four under his co-direction) and, over the years, he has been a lead investigator on federal and state research or research-infrastructure grants totaling more than ten million dollars.

	Tohline earned a B.S. in Physics from [http://www.centenary.edu/ Centenary College of Louisiana] in 1974 and a Ph.D. in [http://www.astro.ucsc.edu/academics/graduates/index.html Astronomy from the University of California, Santa Cruz] in 1978. Before joining the LSU faculty in 1982, Tohline held a J. Willard Gibbs Instructorship in the [http://astronomy.yale.edu/ Astronomy Department at Yale University] and a postdoctoral fellowship at [http://www.lanl.gov/ Los Alamos National Laboratory]. He has served as a member of the [http://www.nsf.gov/mps/former_mpsac_members.jsp Advisory Council for the Directorate of Mathematical & Physical Sciences] of the U.S. National Science Foundation (NSF), as [http://www.nsf.gov/mps/advisory/covdocs/AST_COV_Report_2011_Final.pdf Chair of the Committee of Visitors for the NSF Astronomy Division], as co-editor of the Vizualization Corner for [http://scitation.aip.org/content/aip/journal/cise ''Computing in Science and Engineering''] (a magazine published jointly by the American Institute of Physics and the IEEE Computer Society), as a member of the Applications Strategy Council of [http://www.internet2.edu/ Internet2], on the Program Advisory Council of [http://www.ligo.caltech.edu/ LIGO], as Chairman of [http://www.phys.lsu.edu/newwebsite/ LSU's Department of Physics & Astronomy], and as [https://www.cct.lsu.edu/ Director of LSU's Center for Computation & Technology].		Tohline earned a B.S. in Physics from [http://www.centenary.edu/ Centenary College of Louisiana] in 1974 and a Ph.D. in [http://www.astro.ucsc.edu/academics/graduates/index.html Astronomy from the University of California, Santa Cruz] in 1978. Before joining the LSU faculty in 1982, Tohline held a J. Willard Gibbs Instructorship in the [http://astronomy.yale.edu/ Astronomy Department at Yale University] and a postdoctoral fellowship at [http://www.lanl.gov/ Los Alamos National Laboratory]. He has served as a member of the [http://www.nsf.gov/mps/former_mpsac_members.jsp Advisory Council for the Directorate of Mathematical & Physical Sciences] of the U.S. National Science Foundation (NSF), as [http://www.nsf.gov/mps/advisory/covdocs/AST_COV_Report_2011_Final.pdf Chair of the Committee of Visitors for the NSF Astronomy Division], as co-editor of the Vizualization Corner for [http://scitation.aip.org/content/aip/journal/cise ''Computing in Science and Engineering''] (a magazine published jointly by the American Institute of Physics and the IEEE Computer Society), as a member of the Applications Strategy Council of [http://www.internet2.edu/ Internet2], on the Program Advisory Council of [http://www.ligo.caltech.edu/ LIGO], as Chairman of [http://www.phys.lsu.edu/newwebsite/ LSU's Department of Physics & Astronomy], and as [https://www.cct.lsu.edu/ Director of LSU's Center for Computation & Technology].