Matches in SemOpenAlex for { <https://semopenalex.org/work/W3105113820> ?p ?o ?g. }
- W3105113820 endingPage "701" @default.
- W3105113820 startingPage "693" @default.
- W3105113820 abstract "We present data for 18 blazars observed with ASCA, half of which were also observed contemporaneously with EGRET as parts of multi-wavelength campaigns. The observations show a clear difference in the spectra between three subclasses of blazars, namely the High-energy peaked BL Lac objects (HBLs), Low-energy peaked BL Lac objects (LBLs), and quasar-hosted blazars (QHBs). We find that the radiation process responsible for the HE peak for HBLs can be explained solely by Synchrotron-Self-Compton (SSC) emission, with the Doppler factor consistent with the VLBI and/or gamma-ray variability data. For many QHBs, on the other hand, the gamma-rays cannot be solely due to the SSC mechanism unless the Doppler factor is significantly in excess of that inferred from VLBI data. We consider an alternative scenario consistent with the measured values of the Doppler factor, where the SSC component is still present in QHBs and it dominates in the X-ray band, but it is below the observed gamma-ray spectrum. With an assumption that the peak of the SSC emission is on the extrapolation of the X-ray spectrum, and adopting the Doppler factor of 10, we infer the magnetic field to be 0.1 - 1 Gauss, and Lorentz factors of electrons radiating at the peak of the nu F(nu) spectrum of 10^3 for QHBs; this is much lower than 10^5 for HBLs. This difference is most likely due to the large photon density expected in QHBs." @default.
- W3105113820 created "2020-11-23" @default.
- W3105113820 creator A5013995617 @default.
- W3105113820 creator A5034573525 @default.
- W3105113820 creator A5050905248 @default.
- W3105113820 creator A5051263748 @default.
- W3105113820 creator A5059313768 @default.
- W3105113820 creator A5075199658 @default.
- W3105113820 creator A5089094131 @default.
- W3105113820 date "1998-09-10" @default.
- W3105113820 modified "2023-10-15" @default.
- W3105113820 title "<i>ASCA</i>Observations of Blazars and Multiband Analysis" @default.
- W3105113820 cites W1524618787 @default.
- W3105113820 cites W1612145927 @default.
- W3105113820 cites W1627220256 @default.
- W3105113820 cites W1975294498 @default.
- W3105113820 cites W1978059554 @default.
- W3105113820 cites W1979115990 @default.
- W3105113820 cites W1980450369 @default.
- W3105113820 cites W1981743157 @default.
- W3105113820 cites W1983354252 @default.
- W3105113820 cites W1983650180 @default.
- W3105113820 cites W1986998837 @default.
- W3105113820 cites W1990440936 @default.
- W3105113820 cites W1991136743 @default.
- W3105113820 cites W1991477231 @default.
- W3105113820 cites W1992259562 @default.
- W3105113820 cites W1998710788 @default.
- W3105113820 cites W1998935491 @default.
- W3105113820 cites W2001514823 @default.
- W3105113820 cites W2002015260 @default.
- W3105113820 cites W2003665148 @default.
- W3105113820 cites W2005354006 @default.
- W3105113820 cites W2006920958 @default.
- W3105113820 cites W2008427297 @default.
- W3105113820 cites W2009205983 @default.
- W3105113820 cites W2009682489 @default.
- W3105113820 cites W2011871206 @default.
- W3105113820 cites W2012576437 @default.
- W3105113820 cites W2013094791 @default.
- W3105113820 cites W2015593437 @default.
- W3105113820 cites W2016079907 @default.
- W3105113820 cites W2017396100 @default.
- W3105113820 cites W2023311746 @default.
- W3105113820 cites W2032908778 @default.
- W3105113820 cites W2035248451 @default.
- W3105113820 cites W2037970068 @default.
- W3105113820 cites W2038367995 @default.
- W3105113820 cites W2041963356 @default.
- W3105113820 cites W2044093309 @default.
- W3105113820 cites W2045299794 @default.
- W3105113820 cites W2045377728 @default.
- W3105113820 cites W2047315855 @default.
- W3105113820 cites W2049775896 @default.
- W3105113820 cites W2050276909 @default.
- W3105113820 cites W2052926897 @default.
- W3105113820 cites W2055357571 @default.
- W3105113820 cites W2056577833 @default.
- W3105113820 cites W2056949247 @default.
- W3105113820 cites W2059587447 @default.
- W3105113820 cites W2060871469 @default.
- W3105113820 cites W2063451503 @default.
- W3105113820 cites W2069138912 @default.
- W3105113820 cites W2071065321 @default.
- W3105113820 cites W2073227135 @default.
- W3105113820 cites W2080748776 @default.
- W3105113820 cites W2085128632 @default.
- W3105113820 cites W2085944629 @default.
- W3105113820 cites W2087183011 @default.
- W3105113820 cites W2088868638 @default.
- W3105113820 cites W2089764713 @default.
- W3105113820 cites W2090684783 @default.
- W3105113820 cites W2091057086 @default.
- W3105113820 cites W2103318818 @default.
- W3105113820 cites W2120044719 @default.
- W3105113820 cites W2124633616 @default.
- W3105113820 cites W2132735533 @default.
- W3105113820 cites W2139959405 @default.
- W3105113820 cites W2147307927 @default.
- W3105113820 cites W2152242740 @default.
- W3105113820 cites W2154171423 @default.
- W3105113820 cites W2161055569 @default.
- W3105113820 cites W2170253548 @default.
- W3105113820 cites W2335583047 @default.
- W3105113820 cites W2614483794 @default.
- W3105113820 cites W3012165734 @default.
- W3105113820 cites W3033624324 @default.
- W3105113820 cites W3101015061 @default.
- W3105113820 cites W3101353593 @default.
- W3105113820 cites W3105535499 @default.
- W3105113820 cites W3191356500 @default.
- W3105113820 cites W37960100 @default.
- W3105113820 cites W4233180987 @default.
- W3105113820 cites W4244222148 @default.
- W3105113820 doi "https://doi.org/10.1086/306125" @default.
- W3105113820 hasPublicationYear "1998" @default.
- W3105113820 type Work @default.
- W3105113820 sameAs 3105113820 @default.