FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W3100898951> ?p ?o ?g. }

• W3100898951 endingPage "88" @default.
• W3100898951 startingPage "88" @default.
• W3100898951 abstract "In systems accreting well below the Eddington rate, the plasma in the innermost regions of the disk is collisionless and two-temperature, with the ions hotter than the electrons. Yet, whether a collisionless faster-than-Coulomb energy transfer mechanism exists in two-temperature accretion flows is still an open question. We study the physics of electron heating during the growth of ion velocity-space instabilities, by means of multi-dimensional particle-in-cell (PIC) simulations. A large-scale compression - embedded in a novel form of the PIC equations - continuously amplifies the field. This constantly drives a pressure anisotropy P_perp > P_parallel, due to the adiabatic invariance of the particle magnetic moments. We find that, for ion plasma beta values beta_i ~ 5-30 appropriate for the midplane of low-luminosity accretion flows, mirror modes dominate if the electron-to-proton temperature ratio is > 0.2, whereas if it is < 0.2 the ion cyclotron instability triggers the growth of strong Alfven-like waves, that pitch-angle scatter the ions to maintain marginal stability. We develop an analytical model of electron heating during the growth of the ion cyclotron instability, which we validate with PIC simulations. We find that for cold electrons (beta_e < m_e/m_i), the electron energy gain is controlled by the magnitude of the E-cross-B velocity induced by the ion cyclotron waves. This term is independent of the initial electron temperature, so it provides a solid energy floor even for electrons starting with extremely low temperatures. On the other hand, the electron energy gain for beta_e > m_e/m_i - governed by the conservation of the magnetic moment in the growing fields of the instability - is proportional to the initial electron temperature. Our results have implications for two-temperature accretion flows as well as the solar wind and intracluster plasmas. [abridged]" @default.
• W3100898951 created "2020-11-23" @default.
• W3100898951 creator A5032765567 @default.
• W3100898951 creator A5080658446 @default.
• W3100898951 date "2015-02-12" @default.
• W3100898951 modified "2023-10-18" @default.
• W3100898951 title "ELECTRON HEATING BY THE ION CYCLOTRON INSTABILITY IN COLLISIONLESS ACCRETION FLOWS. I. COMPRESSION-DRIVEN INSTABILITIES AND THE ELECTRON HEATING MECHANISM" @default.
• W3100898951 cites W1499480006 @default.
• W3100898951 cites W1881232094 @default.
• W3100898951 cites W1963734049 @default.
• W3100898951 cites W1970901473 @default.
• W3100898951 cites W1972427024 @default.
• W3100898951 cites W1976168642 @default.
• W3100898951 cites W1981987637 @default.
• W3100898951 cites W1991167125 @default.
• W3100898951 cites W1994057536 @default.
• W3100898951 cites W1994793483 @default.
• W3100898951 cites W1995604961 @default.
• W3100898951 cites W1998925670 @default.
• W3100898951 cites W1999417864 @default.
• W3100898951 cites W2001741999 @default.
• W3100898951 cites W2004939083 @default.
• W3100898951 cites W2005521083 @default.
• W3100898951 cites W2013491657 @default.
• W3100898951 cites W2014489665 @default.
• W3100898951 cites W2015011282 @default.
• W3100898951 cites W2015222572 @default.
• W3100898951 cites W2019788805 @default.
• W3100898951 cites W2027824283 @default.
• W3100898951 cites W2033696809 @default.
• W3100898951 cites W2038398739 @default.
• W3100898951 cites W2038990236 @default.
• W3100898951 cites W2039131488 @default.
• W3100898951 cites W2048673059 @default.
• W3100898951 cites W2049319759 @default.
• W3100898951 cites W2050183901 @default.
• W3100898951 cites W2051205889 @default.
• W3100898951 cites W2051864624 @default.
• W3100898951 cites W2052100039 @default.
• W3100898951 cites W2054280515 @default.
• W3100898951 cites W2054396387 @default.
• W3100898951 cites W2054601427 @default.
• W3100898951 cites W2061041487 @default.
• W3100898951 cites W2062247865 @default.
• W3100898951 cites W2063026166 @default.
• W3100898951 cites W2063606184 @default.
• W3100898951 cites W2064965371 @default.
• W3100898951 cites W2072449268 @default.
• W3100898951 cites W2072483452 @default.
• W3100898951 cites W2075884647 @default.
• W3100898951 cites W2077461433 @default.
• W3100898951 cites W2078965772 @default.
• W3100898951 cites W2079911557 @default.
• W3100898951 cites W2080065741 @default.
• W3100898951 cites W2083379598 @default.
• W3100898951 cites W2084472499 @default.
• W3100898951 cites W2087118423 @default.
• W3100898951 cites W2090272405 @default.
• W3100898951 cites W2098668960 @default.
• W3100898951 cites W2101335960 @default.
• W3100898951 cites W2103540355 @default.
• W3100898951 cites W2109112103 @default.
• W3100898951 cites W2112128229 @default.
• W3100898951 cites W2113540914 @default.
• W3100898951 cites W2115986060 @default.
• W3100898951 cites W2117848361 @default.
• W3100898951 cites W2118913717 @default.
• W3100898951 cites W2135283184 @default.
• W3100898951 cites W2146733852 @default.
• W3100898951 cites W2154591032 @default.
• W3100898951 cites W2155140415 @default.
• W3100898951 cites W2170733202 @default.
• W3100898951 cites W2985443361 @default.
• W3100898951 cites W3099086374 @default.
• W3100898951 cites W3099225611 @default.
• W3100898951 cites W3099635155 @default.
• W3100898951 cites W3099961299 @default.
• W3100898951 cites W3100188330 @default.
• W3100898951 cites W3100307890 @default.
• W3100898951 cites W3100345056 @default.
• W3100898951 cites W3100898951 @default.
• W3100898951 cites W3101418731 @default.
• W3100898951 cites W3101493068 @default.
• W3100898951 cites W3102861481 @default.
• W3100898951 cites W3104031850 @default.
• W3100898951 cites W3105463114 @default.
• W3100898951 cites W3105706072 @default.
• W3100898951 cites W3105945545 @default.
• W3100898951 cites W3106321351 @default.
• W3100898951 doi "https://doi.org/10.1088/0004-637x/800/2/88" @default.
• W3100898951 hasPublicationYear "2015" @default.
• W3100898951 type Work @default.
• W3100898951 sameAs 3100898951 @default.
• W3100898951 citedByCount "73" @default.
• W3100898951 countsByYear W31008989512015 @default.
• W3100898951 countsByYear W31008989512016 @default.
• W3100898951 countsByYear W31008989512017 @default.
• W3100898951 countsByYear W31008989512018 @default.

• next