Abstract
We calculate radio light curves produced by the bow shock that is likely to form in front of the G2 cloud when it penetrates the accretion disc of Sgr A*. The shock acceleration of the radioemitting electrons is captured self-consistently by means of first-principles particle-in-cell simulations. We show that the radio luminosity is expected to reach maximum in early 2013, roughly a month after the bow shock crosses the orbit pericentre. We estimate the peak radio flux at 1.4 GHz to be 1.4-22 Jy depending on the assumed orbit orientation and parameters. We show that the most promising frequencies for radio observations are in the 0.1 < ν < 1 GHz range, for which the bow shock emission will be much stronger than the intrinsic radio flux for all the models considered.
| Original language | English (US) |
|---|---|
| Pages (from-to) | 478-491 |
| Number of pages | 14 |
| Journal | Monthly Notices of the Royal Astronomical Society |
| Volume | 432 |
| Issue number | 1 |
| DOIs | |
| State | Published - Jun 2013 |
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Keywords
- Acceleration of particles
- Accretion, accretion discs
- Black hole physics
- Radiation mechanisms: non-thermal
ASJC Scopus subject areas
- Space and Planetary Science
- Astronomy and Astrophysics
Cite this
Radio light curves during the passage of cloud G2 near Sgr A. / Sadowski, Aleksander; Sironi, Lorenzo; Abarca, David; Guo, Xinyi; Ozel, Feryal; Narayan, Ramesh.
In: Monthly Notices of the Royal Astronomical Society, Vol. 432, No. 1, 06.2013, p. 478-491.Research output: Contribution to journal › Article
}
TY - JOUR
T1 - Radio light curves during the passage of cloud G2 near Sgr A
AU - Sadowski, Aleksander
AU - Sironi, Lorenzo
AU - Abarca, David
AU - Guo, Xinyi
AU - Ozel, Feryal
AU - Narayan, Ramesh
PY - 2013/6
Y1 - 2013/6
N2 - We calculate radio light curves produced by the bow shock that is likely to form in front of the G2 cloud when it penetrates the accretion disc of Sgr A*. The shock acceleration of the radioemitting electrons is captured self-consistently by means of first-principles particle-in-cell simulations. We show that the radio luminosity is expected to reach maximum in early 2013, roughly a month after the bow shock crosses the orbit pericentre. We estimate the peak radio flux at 1.4 GHz to be 1.4-22 Jy depending on the assumed orbit orientation and parameters. We show that the most promising frequencies for radio observations are in the 0.1 < ν < 1 GHz range, for which the bow shock emission will be much stronger than the intrinsic radio flux for all the models considered.
AB - We calculate radio light curves produced by the bow shock that is likely to form in front of the G2 cloud when it penetrates the accretion disc of Sgr A*. The shock acceleration of the radioemitting electrons is captured self-consistently by means of first-principles particle-in-cell simulations. We show that the radio luminosity is expected to reach maximum in early 2013, roughly a month after the bow shock crosses the orbit pericentre. We estimate the peak radio flux at 1.4 GHz to be 1.4-22 Jy depending on the assumed orbit orientation and parameters. We show that the most promising frequencies for radio observations are in the 0.1 < ν < 1 GHz range, for which the bow shock emission will be much stronger than the intrinsic radio flux for all the models considered.
KW - Acceleration of particles
KW - Accretion, accretion discs
KW - Black hole physics
KW - Radiation mechanisms: non-thermal
UR - http://www.scopus.com/inward/record.url?scp=84878384434&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84878384434&partnerID=8YFLogxK
U2 - 10.1093/mnras/stt495
DO - 10.1093/mnras/stt495
M3 - Article
AN - SCOPUS:84878384434
VL - 432
SP - 478
EP - 491
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 1
ER -