Neutrino energy equilibration models
Neutrino energy equilibration by neutrino-electron scattering is studied in four physical models, whose temperatures and densities are representative of stellar collapse conditions when electron scattering may be important. Results of Monte Carlo simulations are presented as data against which appro...
Gespeichert in:
| Veröffentlicht in: | Astrophys. J.; (United States) 1980-07, Vol.239, p.271 |
|---|---|
| Hauptverfasser: | , , , , |
| Format: | Artikel |
| Sprache: | eng |
| Schlagworte: | |
| Online-Zugang: | Volltext |
| Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
| container_end_page | |
|---|---|
| container_issue | |
| container_start_page | 271 |
| container_title | Astrophys. J.; (United States) |
| container_volume | 239 |
| creator | Tubbs, D. L. Weaver, T. A. Bowers, R. L. Wilson, J. R. Schramm, D. N. |
| description | Neutrino energy equilibration by neutrino-electron scattering is studied in four physical models, whose temperatures and densities are representative of stellar collapse conditions when electron scattering may be important. Results of Monte Carlo simulations are presented as data against which approximate transport methods may be tested. The neutrino thermalization rate is initially rapid and approximately exponential, and gradually decreases to a slow approach to equilibrium, suggesting the possibility of using a relaxation scheme to approximate the energy equilibration. However, when these results are compared with Fokker-Planck and thermal relaxation algorithms of the kind that have been widely employed in supernova calculations, substantial discrepancies are found. |
| doi_str_mv | 10.1086/158107 |
| format | Article |
| fullrecord | <record><control><sourceid>crossref_osti_</sourceid><recordid>TN_cdi_crossref_primary_10_1086_158107</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>10_1086_158107</sourcerecordid><originalsourceid>FETCH-LOGICAL-c212t-6fa0ac5e68010f9e99e94bd83604c0bc5d1f2680b01d4aed462ebba8d692fb623</originalsourceid><addsrcrecordid>eNotkE1LxDAYhIMoWFf9DUXEW_VN0qTpURZXhUUvCt5CPt5qZLfRJHvYf2-XCgPDMA9zGEIuKdxSUPKOCkWhOyIVFVw1LRfdMakAoG0k7z5OyVnO34fI-r4i1y-4KymMscYR0-e-xt9d2ASbTAlxrLfR4yafk5PBbDJe_PuCvK8e3pZPzfr18Xl5v24co6w0cjBgnECpgMLQYz-ptV5xCa0D64SnA5tKC9S3Bn0rGVprlJc9G6xkfEGu5t2YS9DZhYLuy8VxRFe07ETXCZigmxlyKeaccNA_KWxN2msK-nCAng_gf1NATAQ</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype></control><display><type>article</type><title>Neutrino energy equilibration models</title><source>Alma/SFX Local Collection</source><creator>Tubbs, D. L. ; Weaver, T. A. ; Bowers, R. L. ; Wilson, J. R. ; Schramm, D. N.</creator><creatorcontrib>Tubbs, D. L. ; Weaver, T. A. ; Bowers, R. L. ; Wilson, J. R. ; Schramm, D. N. ; W. K. Kellogg Radiation Laboratory, California Institute of Technology</creatorcontrib><description>Neutrino energy equilibration by neutrino-electron scattering is studied in four physical models, whose temperatures and densities are representative of stellar collapse conditions when electron scattering may be important. Results of Monte Carlo simulations are presented as data against which approximate transport methods may be tested. The neutrino thermalization rate is initially rapid and approximately exponential, and gradually decreases to a slow approach to equilibrium, suggesting the possibility of using a relaxation scheme to approximate the energy equilibration. However, when these results are compared with Fokker-Planck and thermal relaxation algorithms of the kind that have been widely employed in supernova calculations, substantial discrepancies are found.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.1086/158107</identifier><language>eng</language><publisher>United States</publisher><subject>BOLTZMANN EQUATION ; CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS ; DIFFERENTIAL EQUATIONS ; ELEMENTARY PARTICLES ; ENERGY SPECTRA ; ENERGY TRANSFER ; EQUATIONS ; EQUILIBRIUM ; ERUPTIVE VARIABLE STARS ; FERMIONS ; FLUID MECHANICS ; FOKKER-PLANCK EQUATION ; GRAVITATIONAL COLLAPSE ; HYDRODYNAMICS ; INTERACTIONS ; LEPTON-LEPTON INTERACTIONS ; LEPTONS ; MASSLESS PARTICLES ; MATHEMATICAL MODELS ; MECHANICS ; MONTE CARLO METHOD ; NEUTRINO-ELECTRON INTERACTIONS ; NEUTRINOS ; PARTICLE INTERACTIONS ; SLOWING-DOWN ; SPECTRA ; STAR MODELS ; STARS ; SUPERNOVAE ; THERMALIZATION ; VARIABLE STARS 640102 -- Astrophysics & Cosmology-- Stars & Quasi-Stellar, Radio & X-Ray Sources</subject><ispartof>Astrophys. J.; (United States), 1980-07, Vol.239, p.271</ispartof><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c212t-6fa0ac5e68010f9e99e94bd83604c0bc5d1f2680b01d4aed462ebba8d692fb623</citedby></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>315,782,786,887,27933,27934</link.rule.ids><backlink>$$Uhttps://www.osti.gov/biblio/6757750$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Tubbs, D. L.</creatorcontrib><creatorcontrib>Weaver, T. A.</creatorcontrib><creatorcontrib>Bowers, R. L.</creatorcontrib><creatorcontrib>Wilson, J. R.</creatorcontrib><creatorcontrib>Schramm, D. N.</creatorcontrib><creatorcontrib>W. K. Kellogg Radiation Laboratory, California Institute of Technology</creatorcontrib><title>Neutrino energy equilibration models</title><title>Astrophys. J.; (United States)</title><description>Neutrino energy equilibration by neutrino-electron scattering is studied in four physical models, whose temperatures and densities are representative of stellar collapse conditions when electron scattering may be important. Results of Monte Carlo simulations are presented as data against which approximate transport methods may be tested. The neutrino thermalization rate is initially rapid and approximately exponential, and gradually decreases to a slow approach to equilibrium, suggesting the possibility of using a relaxation scheme to approximate the energy equilibration. However, when these results are compared with Fokker-Planck and thermal relaxation algorithms of the kind that have been widely employed in supernova calculations, substantial discrepancies are found.</description><subject>BOLTZMANN EQUATION</subject><subject>CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS</subject><subject>DIFFERENTIAL EQUATIONS</subject><subject>ELEMENTARY PARTICLES</subject><subject>ENERGY SPECTRA</subject><subject>ENERGY TRANSFER</subject><subject>EQUATIONS</subject><subject>EQUILIBRIUM</subject><subject>ERUPTIVE VARIABLE STARS</subject><subject>FERMIONS</subject><subject>FLUID MECHANICS</subject><subject>FOKKER-PLANCK EQUATION</subject><subject>GRAVITATIONAL COLLAPSE</subject><subject>HYDRODYNAMICS</subject><subject>INTERACTIONS</subject><subject>LEPTON-LEPTON INTERACTIONS</subject><subject>LEPTONS</subject><subject>MASSLESS PARTICLES</subject><subject>MATHEMATICAL MODELS</subject><subject>MECHANICS</subject><subject>MONTE CARLO METHOD</subject><subject>NEUTRINO-ELECTRON INTERACTIONS</subject><subject>NEUTRINOS</subject><subject>PARTICLE INTERACTIONS</subject><subject>SLOWING-DOWN</subject><subject>SPECTRA</subject><subject>STAR MODELS</subject><subject>STARS</subject><subject>SUPERNOVAE</subject><subject>THERMALIZATION</subject><subject>VARIABLE STARS 640102 -- Astrophysics & Cosmology-- Stars & Quasi-Stellar, Radio & X-Ray Sources</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>1980</creationdate><recordtype>article</recordtype><recordid>eNotkE1LxDAYhIMoWFf9DUXEW_VN0qTpURZXhUUvCt5CPt5qZLfRJHvYf2-XCgPDMA9zGEIuKdxSUPKOCkWhOyIVFVw1LRfdMakAoG0k7z5OyVnO34fI-r4i1y-4KymMscYR0-e-xt9d2ASbTAlxrLfR4yafk5PBbDJe_PuCvK8e3pZPzfr18Xl5v24co6w0cjBgnECpgMLQYz-ptV5xCa0D64SnA5tKC9S3Bn0rGVprlJc9G6xkfEGu5t2YS9DZhYLuy8VxRFe07ETXCZigmxlyKeaccNA_KWxN2msK-nCAng_gf1NATAQ</recordid><startdate>19800701</startdate><enddate>19800701</enddate><creator>Tubbs, D. L.</creator><creator>Weaver, T. A.</creator><creator>Bowers, R. L.</creator><creator>Wilson, J. R.</creator><creator>Schramm, D. N.</creator><scope>AAYXX</scope><scope>CITATION</scope><scope>OTOTI</scope></search><sort><creationdate>19800701</creationdate><title>Neutrino energy equilibration models</title><author>Tubbs, D. L. ; Weaver, T. A. ; Bowers, R. L. ; Wilson, J. R. ; Schramm, D. N.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c212t-6fa0ac5e68010f9e99e94bd83604c0bc5d1f2680b01d4aed462ebba8d692fb623</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>1980</creationdate><topic>BOLTZMANN EQUATION</topic><topic>CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS</topic><topic>DIFFERENTIAL EQUATIONS</topic><topic>ELEMENTARY PARTICLES</topic><topic>ENERGY SPECTRA</topic><topic>ENERGY TRANSFER</topic><topic>EQUATIONS</topic><topic>EQUILIBRIUM</topic><topic>ERUPTIVE VARIABLE STARS</topic><topic>FERMIONS</topic><topic>FLUID MECHANICS</topic><topic>FOKKER-PLANCK EQUATION</topic><topic>GRAVITATIONAL COLLAPSE</topic><topic>HYDRODYNAMICS</topic><topic>INTERACTIONS</topic><topic>LEPTON-LEPTON INTERACTIONS</topic><topic>LEPTONS</topic><topic>MASSLESS PARTICLES</topic><topic>MATHEMATICAL MODELS</topic><topic>MECHANICS</topic><topic>MONTE CARLO METHOD</topic><topic>NEUTRINO-ELECTRON INTERACTIONS</topic><topic>NEUTRINOS</topic><topic>PARTICLE INTERACTIONS</topic><topic>SLOWING-DOWN</topic><topic>SPECTRA</topic><topic>STAR MODELS</topic><topic>STARS</topic><topic>SUPERNOVAE</topic><topic>THERMALIZATION</topic><topic>VARIABLE STARS 640102 -- Astrophysics & Cosmology-- Stars & Quasi-Stellar, Radio & X-Ray Sources</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Tubbs, D. L.</creatorcontrib><creatorcontrib>Weaver, T. A.</creatorcontrib><creatorcontrib>Bowers, R. L.</creatorcontrib><creatorcontrib>Wilson, J. R.</creatorcontrib><creatorcontrib>Schramm, D. N.</creatorcontrib><creatorcontrib>W. K. Kellogg Radiation Laboratory, California Institute of Technology</creatorcontrib><collection>CrossRef</collection><collection>OSTI.GOV</collection><jtitle>Astrophys. J.; (United States)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Tubbs, D. L.</au><au>Weaver, T. A.</au><au>Bowers, R. L.</au><au>Wilson, J. R.</au><au>Schramm, D. N.</au><aucorp>W. K. Kellogg Radiation Laboratory, California Institute of Technology</aucorp><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Neutrino energy equilibration models</atitle><jtitle>Astrophys. J.; (United States)</jtitle><date>1980-07-01</date><risdate>1980</risdate><volume>239</volume><spage>271</spage><pages>271-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>Neutrino energy equilibration by neutrino-electron scattering is studied in four physical models, whose temperatures and densities are representative of stellar collapse conditions when electron scattering may be important. Results of Monte Carlo simulations are presented as data against which approximate transport methods may be tested. The neutrino thermalization rate is initially rapid and approximately exponential, and gradually decreases to a slow approach to equilibrium, suggesting the possibility of using a relaxation scheme to approximate the energy equilibration. However, when these results are compared with Fokker-Planck and thermal relaxation algorithms of the kind that have been widely employed in supernova calculations, substantial discrepancies are found.</abstract><cop>United States</cop><doi>10.1086/158107</doi><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0004-637X |
| ispartof | Astrophys. J.; (United States), 1980-07, Vol.239, p.271 |
| issn | 0004-637X 1538-4357 |
| language | eng |
| recordid | cdi_crossref_primary_10_1086_158107 |
| source | Alma/SFX Local Collection |
| subjects | BOLTZMANN EQUATION CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS DIFFERENTIAL EQUATIONS ELEMENTARY PARTICLES ENERGY SPECTRA ENERGY TRANSFER EQUATIONS EQUILIBRIUM ERUPTIVE VARIABLE STARS FERMIONS FLUID MECHANICS FOKKER-PLANCK EQUATION GRAVITATIONAL COLLAPSE HYDRODYNAMICS INTERACTIONS LEPTON-LEPTON INTERACTIONS LEPTONS MASSLESS PARTICLES MATHEMATICAL MODELS MECHANICS MONTE CARLO METHOD NEUTRINO-ELECTRON INTERACTIONS NEUTRINOS PARTICLE INTERACTIONS SLOWING-DOWN SPECTRA STAR MODELS STARS SUPERNOVAE THERMALIZATION VARIABLE STARS 640102 -- Astrophysics & Cosmology-- Stars & Quasi-Stellar, Radio & X-Ray Sources |
| title | Neutrino energy equilibration models |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2024-12-02T17%3A54%3A35IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-crossref_osti_&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Neutrino%20energy%20equilibration%20models&rft.jtitle=Astrophys.%20J.;%20(United%20States)&rft.au=Tubbs,%20D.%20L.&rft.aucorp=W.%20K.%20Kellogg%20Radiation%20Laboratory,%20California%20Institute%20of%20Technology&rft.date=1980-07-01&rft.volume=239&rft.spage=271&rft.pages=271-&rft.issn=0004-637X&rft.eissn=1538-4357&rft_id=info:doi/10.1086/158107&rft_dat=%3Ccrossref_osti_%3E10_1086_158107%3C/crossref_osti_%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_id=info:pmid/&rfr_iscdi=true |