منابع مشابه
TeV emission from SN 1006
Supernova 1006 is the first shell type super-nova remnant to show evidence of particle acceleration to TeV energies. In the present paper we examine this possibility by modeling the observed X-ray non-thermal emission in terms of synchrotron radiation from Fermi accelerated electrons. The predicted synchrotron spectrum fits the radio and non-thermal component of the observed soft X-ray to hard ...
متن کاملOn the origin of TeV radiation of SN 1006
We discuss the link between the nonthermal X-radiation and TeV γ-ray emission from SN 1006, and study the capabilities of both electronic and nucleonic models for explanation of the TeV flux observed from the northeast rim of SN 1006. We show that the interpretation of the TeV radiation by the inverse Compton scattering of electrons on 2.7 K cosmic microwave background radiation is possible, ho...
متن کاملSpatial structure of X - ray filaments in SN 1006
The theory of non-linear diffusive shock acceleration (NLDSA) predicts the formation of a precursor upstream of the shock, where accelerated particles diffuse and induce magnetic field amplification (MFA) through streaming instability. The non-detection of this precursor in X-rays in Chandra observations of the north-eastern region of SN 1006 (G329.6+14.6) led the authors of some previous work ...
متن کاملThe Optical Spectrum of the Sn 1006 Supernova Remnant Revisited
We present the deepest optical spectrum acquired to date of Balmer-dominated shocks in the NW rim of SN 1006. We detect the broad and narrow components of Hα, Hβ and Hγ and report the first detection of the He I λ 6678 emission line in this supernova remnant. We may have detected, at the 1.5σ level, faint He II λ4686 emission. We measure a full width half maximum of 2290± 80 km s in the broad c...
متن کاملSlow temperature equilibration behind the shock front of SN 1006
We report on the observation of O VII Doppler line broadening in a compact knot at the edge of SN 1006 detected with the Reflective Grating Spectrometer on board XMM-Newton. The observed line width of σ = 3.4± 0.5 eV at a line energy of 574 eV indicates an oxygen temperature of kT = 528± 150 keV. Combined with the observed electron temperature of ∼ 1.5 keV the observed broadening is direct evid...
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ژورنال
عنوان ژورنال: Publications of the Astronomical Society of Japan
سال: 2008
ISSN: 0004-6264,2053-051X
DOI: 10.1093/pasj/60.sp1.s153