Radio light curves during the passage of cloud G2 near Sgr A

被引:39
作者
Sadowski, Aleksander [1 ]
Sironi, Lorenzo [1 ]
Abarca, David [2 ]
Guo, Xinyi [1 ]
Ozel, Feryal [1 ,3 ]
Narayan, Ramesh [1 ]
机构
[1] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
[2] Harvard Univ, Cambridge, MA 02138 USA
[3] Univ Arizona, Tucson, AZ 85721 USA
基金
美国国家科学基金会;
关键词
acceleration of particles; accretion; accretion discs; black hole physics; radiation mechanisms: non-thermal; SAGITTARIUS-A-ASTERISK; ADVECTION-DOMINATED ACCRETION; GENERAL-RELATIVISTIC MAGNETOHYDRODYNAMICS; BLACK-HOLE; GALACTIC-CENTER; X-RAY; PARTICLE-ACCELERATION; NUMERICAL-SIMULATION; GRMHD SIMULATIONS; SHOCKS;
D O I
10.1093/mnras/stt495
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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 radio-emitting 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 < nu < 1 GHz range, for which the bow shock emission will be much stronger than the intrinsic radio flux for all the models considered.
引用
收藏
页码:478 / 491
页数:14
相关论文
共 45 条
  • [1] COSMOS++:: Relativistic magnetohydrodynamics on unstructured grids with local adaptive refinement
    Anninos, P
    Fragile, PC
    Salmonson, JD
    [J]. ASTROPHYSICAL JOURNAL, 2005, 635 (01) : 723 - 740
  • [2] [Anonymous], 1979, Radiative Processes in Astrophysics
  • [3] Chandra X-ray spectroscopic imaging of Sagittarius A* and the central parsec of the Galaxy
    Baganoff, FK
    Maeda, Y
    Morris, M
    Bautz, MW
    Brandt, WN
    Cui, W
    Doty, JP
    Feigelson, ED
    Garmire, GP
    Pravdo, SH
    Ricker, GR
    Townsley, LK
    [J]. ASTROPHYSICAL JOURNAL, 2003, 591 (02) : 891 - 915
  • [4] Rapid X-ray flaring from the direction of the supermassive black hole at the Galactic Centre
    Baganoff, FK
    Bautz, MW
    Brandt, WN
    Chartas, G
    Feigelson, ED
    Garmire, GP
    Maeda, Y
    Morris, M
    Ricker, GR
    Townsley, LK
    Walter, F
    [J]. NATURE, 2001, 413 (6851) : 45 - 48
  • [5] EVIDENCE FOR WARPED DISKS OF YOUNG STARS IN THE GALACTIC CENTER
    Bartko, H.
    Martins, F.
    Fritz, T. K.
    Genzel, R.
    Levin, Y.
    Perets, H. B.
    Paumard, T.
    Nayakshin, S.
    Gerhard, O.
    Alexander, T.
    Dodds-Eden, K.
    Eisenhauer, F.
    Gillessen, S.
    Mascetti, L.
    Ott, T.
    Perrin, G.
    Pfuhl, O.
    Reid, M. J.
    Rouan, D.
    Sternberg, A.
    Trippe, S.
    [J]. ASTROPHYSICAL JOURNAL, 2009, 697 (02) : 1741 - 1763
  • [6] SHOCK-DRIFT PARTICLE-ACCELERATION IN SUPERLUMINAL SHOCKS - A MODEL FOR HOT SPOTS IN EXTRAGALACTIC RADIO-SOURCES
    BEGELMAN, MC
    KIRK, JG
    [J]. ASTROPHYSICAL JOURNAL, 1990, 353 (01) : 66 - 80
  • [7] PARTICLE-ACCELERATION AT ASTROPHYSICAL SHOCKS - A THEORY OF COSMIC-RAY ORIGIN
    BLANDFORD, R
    EICHLER, D
    [J]. PHYSICS REPORTS-REVIEW SECTION OF PHYSICS LETTERS, 1987, 154 (01): : 1 - 75
  • [8] EVIDENCE FOR LOW BLACK HOLE SPIN AND PHYSICALLY MOTIVATED ACCRETION MODELS FROM MILLIMETER-VLBI OBSERVATIONS OF SAGITTARIUS A*
    Broderick, Avery E.
    Fish, Vincent L.
    Doeleman, Sheperd S.
    Loeb, Abraham
    [J]. ASTROPHYSICAL JOURNAL, 2011, 735 (02)
  • [9] MHD SIMULATIONS OF ACCRETION ONTO Sgr A*: QUIESCENT FLUCTUATIONS, OUTBURSTS, AND QUASIPERIODICITY
    Chan, Chi-Kwan
    Liu, Siming
    Fryer, Christopher L.
    Psaltis, Dimitrios
    Oezel, Feryal
    Rockefeller, Gabriel
    Melia, Fulvio
    [J]. ASTROPHYSICAL JOURNAL, 2009, 701 (01) : 521 - 534
  • [10] RADIO-SOURCE AT GALACTIC NUCLEUS
    DAVIES, RD
    WALSH, D
    BOOTH, RS
    [J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 1976, 177 (02) : 319 - 333