TIME-DEPENDENT STOCHASTIC ACCELERATION MODEL FOR FERMI BUBBLES
ABSTRACT We study stochastic acceleration models for the Fermi bubbles. Turbulence is excited just behind the shock front via Kelvin-Helmholtz, Rayleigh-Taylor, or Richtmyer-Meshkov instabilities, and plasma particles are continuously accelerated by the interaction with the turbulence. The turbulenc...
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| Veröffentlicht in: | The Astrophysical journal 2015-12, Vol.814 (2), p.1-9 |
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| creator | Sasaki, Kento Asano, Katsuaki Terasawa, Toshio |
| description | ABSTRACT We study stochastic acceleration models for the Fermi bubbles. Turbulence is excited just behind the shock front via Kelvin-Helmholtz, Rayleigh-Taylor, or Richtmyer-Meshkov instabilities, and plasma particles are continuously accelerated by the interaction with the turbulence. The turbulence gradually decays as it goes away from the shock fronts. Adopting a phenomenological model for the stochastic acceleration, we explicitly solve the temporal evolution of the particle energy distribution in the turbulence. Our results show that the spatial distribution of high-energy particles is different from those for a steady solution. We also show that the contribution of electrons that escaped from the acceleration regions significantly softens the photon spectrum. The photon spectrum and surface brightness profile are reproduced by our models. If the escape efficiency is very high, the radio flux from the escaped low-energy electrons can be comparable to that of the WMAP haze. We also demonstrate hadronic models with the stochastic acceleration, but they are unlikely in the viewpoint of the energy budget. |
| doi_str_mv | 10.1088/0004-637X/814/2/93 |
| format | Article |
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Turbulence is excited just behind the shock front via Kelvin-Helmholtz, Rayleigh-Taylor, or Richtmyer-Meshkov instabilities, and plasma particles are continuously accelerated by the interaction with the turbulence. The turbulence gradually decays as it goes away from the shock fronts. Adopting a phenomenological model for the stochastic acceleration, we explicitly solve the temporal evolution of the particle energy distribution in the turbulence. Our results show that the spatial distribution of high-energy particles is different from those for a steady solution. We also show that the contribution of electrons that escaped from the acceleration regions significantly softens the photon spectrum. The photon spectrum and surface brightness profile are reproduced by our models. If the escape efficiency is very high, the radio flux from the escaped low-energy electrons can be comparable to that of the WMAP haze. We also demonstrate hadronic models with the stochastic acceleration, but they are unlikely in the viewpoint of the energy budget.</description><identifier>ISSN: 0004-637X</identifier><identifier>ISSN: 1538-4357</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.1088/0004-637X/814/2/93</identifier><language>eng</language><publisher>United States: The American Astronomical Society</publisher><subject>ACCELERATION ; acceleration of particles ; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ; BRIGHTNESS ; BUBBLES ; COMPARATIVE EVALUATIONS ; Computational fluid dynamics ; cosmic rays ; ENERGY SPECTRA ; Fluid flow ; GALAXIES ; Galaxy: center ; GAMMA RADIATION ; gamma rays: ISM ; HELMHOLTZ INSTABILITY ; Photons ; PLASMA ; radiation mechanisms: non-thermal ; RAYLEIGH-TAYLOR INSTABILITY ; SPATIAL DISTRIBUTION ; STOCHASTIC PROCESSES ; Stochasticity ; SURFACES ; TIME DEPENDENCE ; TURBULENCE ; Turbulent flow</subject><ispartof>The Astrophysical journal, 2015-12, Vol.814 (2), p.1-9</ispartof><rights>2015. The American Astronomical Society. All rights reserved.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c490t-af720fffdd4eca7641b716fed0697053065c38084aa1f31da5a0ed7cfd268f2d3</citedby><cites>FETCH-LOGICAL-c490t-af720fffdd4eca7641b716fed0697053065c38084aa1f31da5a0ed7cfd268f2d3</cites><orcidid>0000-0001-9064-160X</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.1088/0004-637X/814/2/93/pdf$$EPDF$$P50$$Giop$$H</linktopdf><link.rule.ids>230,314,780,784,885,27924,27925,38890,53867</link.rule.ids><linktorsrc>$$Uhttps://iopscience.iop.org/article/10.1088/0004-637X/814/2/93$$EView_record_in_IOP_Publishing$$FView_record_in_$$GIOP_Publishing</linktorsrc><backlink>$$Uhttps://www.osti.gov/biblio/22521866$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Sasaki, Kento</creatorcontrib><creatorcontrib>Asano, Katsuaki</creatorcontrib><creatorcontrib>Terasawa, Toshio</creatorcontrib><title>TIME-DEPENDENT STOCHASTIC ACCELERATION MODEL FOR FERMI BUBBLES</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>ABSTRACT We study stochastic acceleration models for the Fermi bubbles. Turbulence is excited just behind the shock front via Kelvin-Helmholtz, Rayleigh-Taylor, or Richtmyer-Meshkov instabilities, and plasma particles are continuously accelerated by the interaction with the turbulence. The turbulence gradually decays as it goes away from the shock fronts. Adopting a phenomenological model for the stochastic acceleration, we explicitly solve the temporal evolution of the particle energy distribution in the turbulence. Our results show that the spatial distribution of high-energy particles is different from those for a steady solution. We also show that the contribution of electrons that escaped from the acceleration regions significantly softens the photon spectrum. The photon spectrum and surface brightness profile are reproduced by our models. If the escape efficiency is very high, the radio flux from the escaped low-energy electrons can be comparable to that of the WMAP haze. We also demonstrate hadronic models with the stochastic acceleration, but they are unlikely in the viewpoint of the energy budget.</description><subject>ACCELERATION</subject><subject>acceleration of particles</subject><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</subject><subject>BRIGHTNESS</subject><subject>BUBBLES</subject><subject>COMPARATIVE EVALUATIONS</subject><subject>Computational fluid dynamics</subject><subject>cosmic rays</subject><subject>ENERGY SPECTRA</subject><subject>Fluid flow</subject><subject>GALAXIES</subject><subject>Galaxy: center</subject><subject>GAMMA RADIATION</subject><subject>gamma rays: ISM</subject><subject>HELMHOLTZ INSTABILITY</subject><subject>Photons</subject><subject>PLASMA</subject><subject>radiation mechanisms: non-thermal</subject><subject>RAYLEIGH-TAYLOR INSTABILITY</subject><subject>SPATIAL DISTRIBUTION</subject><subject>STOCHASTIC PROCESSES</subject><subject>Stochasticity</subject><subject>SURFACES</subject><subject>TIME DEPENDENCE</subject><subject>TURBULENCE</subject><subject>Turbulent flow</subject><issn>0004-637X</issn><issn>1538-4357</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2015</creationdate><recordtype>article</recordtype><recordid>eNqNkM9LwzAUgIMoOKf_gKeCFy9d86tpchG2LtNCt8rWgbcQ0wQ7tnU23cH_3o6JR_H0ePB9D94HwD2CIwQ5jyCENGQkeYs4ohGOBLkAAxQTHlISJ5dg8AtcgxvvN6cVCzEAT2U2l-FUvsrFVC7KYFUW6ct4VWZpME5TmcvluMyKRTAvpjIPZsUymMnlPAsm68kkl6tbcOX01tu7nzkE65ks05cwL56zdJyHhgrYhdolGDrnqopaoxNG0XuCmLMVZCKBMYEsNoRDTrVGjqBKxxraKjGuwow7XJEheDjfbXxXK2_qzpoP0-z31nQK4xgjzlhPPZ6pQ9t8Hq3v1K72xm63em-bo1eII9b_zcg_0ERAQYSgtEfxGTVt431rnTq09U63XwpBdaqvTjXVKa7q6yusBOml0Vmqm4PaNMd23-f5S_gGVfV-UQ</recordid><startdate>20151201</startdate><enddate>20151201</enddate><creator>Sasaki, Kento</creator><creator>Asano, Katsuaki</creator><creator>Terasawa, Toshio</creator><general>The American Astronomical Society</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>KL.</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>OTOTI</scope><orcidid>https://orcid.org/0000-0001-9064-160X</orcidid></search><sort><creationdate>20151201</creationdate><title>TIME-DEPENDENT STOCHASTIC ACCELERATION MODEL FOR FERMI BUBBLES</title><author>Sasaki, Kento ; Asano, Katsuaki ; Terasawa, Toshio</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c490t-af720fffdd4eca7641b716fed0697053065c38084aa1f31da5a0ed7cfd268f2d3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2015</creationdate><topic>ACCELERATION</topic><topic>acceleration of particles</topic><topic>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</topic><topic>BRIGHTNESS</topic><topic>BUBBLES</topic><topic>COMPARATIVE EVALUATIONS</topic><topic>Computational fluid dynamics</topic><topic>cosmic rays</topic><topic>ENERGY SPECTRA</topic><topic>Fluid flow</topic><topic>GALAXIES</topic><topic>Galaxy: center</topic><topic>GAMMA RADIATION</topic><topic>gamma rays: ISM</topic><topic>HELMHOLTZ INSTABILITY</topic><topic>Photons</topic><topic>PLASMA</topic><topic>radiation mechanisms: non-thermal</topic><topic>RAYLEIGH-TAYLOR INSTABILITY</topic><topic>SPATIAL DISTRIBUTION</topic><topic>STOCHASTIC PROCESSES</topic><topic>Stochasticity</topic><topic>SURFACES</topic><topic>TIME DEPENDENCE</topic><topic>TURBULENCE</topic><topic>Turbulent flow</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Sasaki, Kento</creatorcontrib><creatorcontrib>Asano, Katsuaki</creatorcontrib><creatorcontrib>Terasawa, Toshio</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>OSTI.GOV</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Sasaki, Kento</au><au>Asano, Katsuaki</au><au>Terasawa, Toshio</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>TIME-DEPENDENT STOCHASTIC ACCELERATION MODEL FOR FERMI BUBBLES</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2015-12-01</date><risdate>2015</risdate><volume>814</volume><issue>2</issue><spage>1</spage><epage>9</epage><pages>1-9</pages><issn>0004-637X</issn><issn>1538-4357</issn><eissn>1538-4357</eissn><abstract>ABSTRACT We study stochastic acceleration models for the Fermi bubbles. Turbulence is excited just behind the shock front via Kelvin-Helmholtz, Rayleigh-Taylor, or Richtmyer-Meshkov instabilities, and plasma particles are continuously accelerated by the interaction with the turbulence. The turbulence gradually decays as it goes away from the shock fronts. Adopting a phenomenological model for the stochastic acceleration, we explicitly solve the temporal evolution of the particle energy distribution in the turbulence. Our results show that the spatial distribution of high-energy particles is different from those for a steady solution. We also show that the contribution of electrons that escaped from the acceleration regions significantly softens the photon spectrum. The photon spectrum and surface brightness profile are reproduced by our models. If the escape efficiency is very high, the radio flux from the escaped low-energy electrons can be comparable to that of the WMAP haze. We also demonstrate hadronic models with the stochastic acceleration, but they are unlikely in the viewpoint of the energy budget.</abstract><cop>United States</cop><pub>The American Astronomical Society</pub><doi>10.1088/0004-637X/814/2/93</doi><tpages>9</tpages><orcidid>https://orcid.org/0000-0001-9064-160X</orcidid><oa>free_for_read</oa></addata></record> |
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| subjects | ACCELERATION acceleration of particles ASTROPHYSICS, COSMOLOGY AND ASTRONOMY BRIGHTNESS BUBBLES COMPARATIVE EVALUATIONS Computational fluid dynamics cosmic rays ENERGY SPECTRA Fluid flow GALAXIES Galaxy: center GAMMA RADIATION gamma rays: ISM HELMHOLTZ INSTABILITY Photons PLASMA radiation mechanisms: non-thermal RAYLEIGH-TAYLOR INSTABILITY SPATIAL DISTRIBUTION STOCHASTIC PROCESSES Stochasticity SURFACES TIME DEPENDENCE TURBULENCE Turbulent flow |
| title | TIME-DEPENDENT STOCHASTIC ACCELERATION MODEL FOR FERMI BUBBLES |
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