dc.contributor.author |
Paliya, Vaidehi S |
|
dc.contributor.author |
Böttcher, M |
|
dc.contributor.author |
Gurwell, Mark |
|
dc.contributor.author |
Stalin, C. S |
|
dc.date.accessioned |
2021-12-16T04:05:46Z |
|
dc.date.available |
2021-12-16T04:05:46Z |
|
dc.date.issued |
2021-12 |
|
dc.identifier.citation |
The Astrophysical Journal Supplement Series, Vol. 257, No. 2, 37 |
en_US |
dc.identifier.issn |
0067-0049 |
|
dc.identifier.uri |
http://hdl.handle.net/2248/7885 |
|
dc.description |
Restricted Access |
en_US |
dc.description.abstract |
The origin of γ-ray flares observed from blazars is one of the major mysteries in jet physics. We have attempted to
address this problem following a novel spectral energy distribution (SED) fitting technique that explored the flaring
patterns identified in the broadband SEDs of two γ-ray bright blazars, 3C 279 (z = 0.54) and 3C 454.3 (z = 0.86),
using near-simultaneous radio-to-γ-ray observations. For both sources, the γ-ray flux strongly correlates with the
separation of the SED peaks and the Compton dominance. We propose that spectral hardening of the radiating
electron population and/or enhancement of the Doppler factor can naturally explain these observations. In both
cases, magnetic reconnection may play a pivotal role in powering the luminous γ-ray flares. |
en_US |
dc.language.iso |
en |
en_US |
dc.publisher |
IOP Publishing |
en_US |
dc.relation.uri |
https://doi.org/10.3847/1538-4365/ac365d |
|
dc.rights |
© American Astronomical Society |
|
dc.subject |
Relativistic jets |
en_US |
dc.subject |
Blazars |
en_US |
dc.subject |
Gamma ray astronomy |
en_US |
dc.subject |
Radiative processes |
en_US |
dc.title |
On the Origin of Gamma-Ray Flares from Bright Fermi Blazars |
en_US |
dc.type |
Article |
en_US |