A1 Vertaisarvioitu alkuperäisartikkeli tieteellisessä lehdessä
Investigating the Mini and Giant Radio Flare Episodes of Cygnus X-3
Tekijät: Egron E, Pellizzoni A, Righini S, Giroletti M, Koljonen K, Pottschmidt K, Trushkin S, Lobina J, Pilia M, Wilms J, Corbel S, Grinberg V, Loru S, Trois A, Rodriguez J, Lahteenmaki A, Tornikoski M, Enestam S, Jarvela E, Jarvela E
Kustantaja: IOP PUBLISHING LTD
Julkaisuvuosi: 2021
Journal: Astrophysical Journal
Tietokannassa oleva lehden nimi: ASTROPHYSICAL JOURNAL
Lehden akronyymi: ASTROPHYS J
Artikkelin numero: ARTN 10
Vuosikerta: 906
Numero: 1
Sivujen määrä: 9
ISSN: 0004-637X
eISSN: 1538-4357
DOI: https://doi.org/10.3847/1538-4357/abc5b1
Rinnakkaistallenteen osoite: https://research.utu.fi/converis/portal/detail/Publication/53028285
The microquasar Cygnus X-3 underwent a giant radio flare in 2017 April, reaching a maximum flux of similar to 16.5 Jy at 8.5 GHz. We present results from a long monitoring campaign carried out with Medicina at 8.5, 18.6, and 24.1 GHz, parallel to the Metsahovi radio telescope at 37 GHz, from 2017 April 4 to 11. We observe a spectral steepening from alpha = 0.2 to 0.5 (with S-nu proportional to nu(-alpha)) within 6 hr of the epoch of the flare's peak maximum, and rapid changes in the spectral slope in the following days during brief enhanced emission episodes while the general trend of the radio flux density indicated the decay of the giant flare. We further study the radio orbital modulation of Cyg X-3 emission associated with the 2017 giant flare and with six mini-flares observed in 1983, 1985, 1994, 1995, 2002, and 2016. The enhanced emission episodes observed during the decline of the giant flare at 8.5 GHz coincide with the orbital phase phi similar to 0.5 (orbital inferior conjunction). On the other hand, the light curves of the mini-flares observed at 15-22 GHz peak at phi similar to 0, except for the 2016 light curve, which is shifted 0.5 w.r.t. the other ones. We attribute the apparent phase shift to the variable location of the emitting region along the bent jet. This might be explained by the different accretion states of the flaring episodes (the 2016 mini-flare occurred in the hypersoft X-ray state).
Ladattava julkaisu This is an electronic reprint of the original article. |  |
