Abstract
We extend and reconcile recent work on turbulence and particle heating in advection-dominated accretion flows. For approximately equipartition magnetic fields, the turbulence primarily heats the electrons. For weaker magnetic fields, the protons are primarily heated. The division between electron and proton heating occurs between β ∼ 5 and β ∼ 100 (β is the ratio of gas to magnetic pressure), depending on unknown details of how Alfvén waves are converted into whistlers on scales of the proton Larmor radius. We also discuss the possibility that magnetic reconnection could be a significant source of electron heating.
Original language | English (US) |
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Pages (from-to) | 248-255 |
Number of pages | 8 |
Journal | Astrophysical Journal |
Volume | 520 |
Issue number | 1 PART 1 |
State | Published - Jul 20 1999 |
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Keywords
- Accretion
- Accretion disks
- MHD
- Plasmas
- Turbulence
ASJC Scopus subject areas
- Space and Planetary Science
Cite this
Turbulence and particle heating in advection-dominated accretion flows. / Quataert, Eliot; Gruzinov, Andrei.
In: Astrophysical Journal, Vol. 520, No. 1 PART 1, 20.07.1999, p. 248-255.Research output: Contribution to journal › Article
}
TY - JOUR
T1 - Turbulence and particle heating in advection-dominated accretion flows
AU - Quataert, Eliot
AU - Gruzinov, Andrei
PY - 1999/7/20
Y1 - 1999/7/20
N2 - We extend and reconcile recent work on turbulence and particle heating in advection-dominated accretion flows. For approximately equipartition magnetic fields, the turbulence primarily heats the electrons. For weaker magnetic fields, the protons are primarily heated. The division between electron and proton heating occurs between β ∼ 5 and β ∼ 100 (β is the ratio of gas to magnetic pressure), depending on unknown details of how Alfvén waves are converted into whistlers on scales of the proton Larmor radius. We also discuss the possibility that magnetic reconnection could be a significant source of electron heating.
AB - We extend and reconcile recent work on turbulence and particle heating in advection-dominated accretion flows. For approximately equipartition magnetic fields, the turbulence primarily heats the electrons. For weaker magnetic fields, the protons are primarily heated. The division between electron and proton heating occurs between β ∼ 5 and β ∼ 100 (β is the ratio of gas to magnetic pressure), depending on unknown details of how Alfvén waves are converted into whistlers on scales of the proton Larmor radius. We also discuss the possibility that magnetic reconnection could be a significant source of electron heating.
KW - Accretion
KW - Accretion disks
KW - MHD
KW - Plasmas
KW - Turbulence
UR - http://www.scopus.com/inward/record.url?scp=0033587426&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=0033587426&partnerID=8YFLogxK
M3 - Article
AN - SCOPUS:0033587426
VL - 520
SP - 248
EP - 255
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1 PART 1
ER -