A time dependent approach to model X-ray and γ–ray light curves of Mrk 421 observed during the flare in February 2010 |
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| Institution: | 1. Astrophysical Sciences Division, Bhabha Atomic Research Center, Mumbai 400 085, India;2. Department of High Energy Physics, Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400 005, India;1. Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL, USA;2. Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba, Japan;3. Department of Physics, University of Adelaide, Adelaide, SA, Australia;4. Dipartimento di Fisica, Università di Torino and INFN Torino, Torino, Italy;5. RIKEN Advanced Science Institute, Wako, Saitama, Japan;6. Palacky University, RCPTM, Olomouc, Czech Republic;7. Institute of Physics of the Academy of Sciences of the Czech Republic, Prague, Czech Republic;8. High Energy Astrophysics Institute and Department of Physics and Astronomy, University of Utah, Salt Lake City, Utah, USA;9. Graduate School of Science, Osaka City University, Osaka, Osaka, Japan;1. Department of Applied Mathematics, Faculty of Mathematical Sciences, Ferdowsi University of Mashhad, Mashhad, Iran;2. Department of Mathematics, Faculty of Mathematics, University of Sistan and Baluchestan, Zahedan, Iran;1. School of Physics and Electronic Engineering, Sichuan University of Science & Engineering, Zigong, 643000, China;2. Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, China;1. Physics Department, McGill University, Montreal, QC H3A 2T8, Canada;2. Department of Physics, Washington University, St. Louis, MO 63130, USA;3. Fred Lawrence Whipple Observatory, Harvard-Smithsonian Center for Astrophysics, Amado, AZ 85645, USA;4. Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA;5. School of Physics, University College Dublin, Belfield, Dublin 4, Ireland;6. Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, CA 95064, USA;7. InVisage Technologies, Inc., Menlo Park, CA 94025, USA;8. Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA;9. Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA;10. School of Physics, National University of Ireland Galway, University Road, Galway, Ireland;11. Department of Physics and Astronomy, Purdue University, West Lafayette, IN 47907, USA;12. Department of Physics and Center for Astrophysics, Tsinghua University, Beijing 100084, China;13. Department of Astronomy and Astrophysics, 525 Davey Lab, Pennsylvania State University, University Park, PA 16802, USA;14. DESY, Platanenallee 6, 15738 Zeuthen, Germany;15. School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA;p. Department of Physics, California State University, East Bay, Hayward, CA 94542, USA;q. Department of Physics and Astronomy and the Bartol Research Institute, University of Delaware, Newark, DE 19716, USA;r. Physics Department, Columbia University, New York, NY 10027, USA;s. Department of Physics and Astronomy, University of Iowa, Van Allen Hall, Iowa City, IA 52242, USA;t. Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA;u. Department of Physics and Astronomy, DePauw University, Greencastle, IN 46135-0037, USA;v. Department of Physics and Astronomy, Barnard College, Columbia University, NY 10027, USA;w. School of Physics and Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street NW, Atlanta, GA 30332-0430, USA;x. Enrico Fermi Institute, University of Chicago, Chicago, IL 60637, USA;y. Institute of Physics and Astronomy, University of Potsdam, 14476 Potsdam-Golm, Germany;z. Department of Physical Sciences, Cork Institute of Technology, Bishopstown, Cork, Ireland |
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| Abstract: | Strong X-ray and γ–ray flares have been detected in February 2010 from the high synchrotron peaked blazar Mrk 421 (z = 0.031). With the motivation of understanding the physics involved in this flaring activity, we study the variability of the source in X-ray and γ–ray energy bands during the period February 10–23, 2010 (MJD 55237–55250). We use near simultaneous X-ray data collected by MAXI, Swift-XRT and γ–ray data collected by Fermi-LAT and TACTIC along with the optical V-band observations by SPOL at Steward Observatory. We observe that the variation in the one day averaged flux from the source during the flare is characterized by fast rise and slow decay. Besides, the TeV γ–ray flux shows a strong correlation with the X-ray flux, suggesting the former to be an outcome of synchrotron self Compton emission process. To model the observed X-ray and γ–ray light curves, we numerically solve the kinetic equation describing the evolution of particle distribution in the emission region. The injection of particle distribution into the emission region, from the putative acceleration region, is assumed to be a time dependent power law. The synchrotron and synchrotron self Compton emission from the evolving particle distribution in the emission region are used to reproduce the X-ray and γ–ray flares successfully. Our study suggests that the flaring activity of Mrk 421 can be an outcome of an efficient acceleration process associated with the increase in underlying non-thermal particle distribution. |
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