Color variability of quasars

Details Color variability of quasars Color variability of quasars

Sep 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...224..812b&link_type=abstract

Astrophysical Journal, Part 1, vol. 224, Sept. 15, 1978, p. 812-815.

Astronomy and Astrophysics

Astrophysics

2

Astronomical Models, Astronomical Photometry, Quasars, Ubv Spectra, Pulsars, Regression Analysis, Supernovae, Variability

Scientific paper

The technique of multiple polynomial regression is employed to search for lack of simultaneity of flareups of quasars and BL Lacertae objects as viewed in different colors, using the multicolor (UBV) photometric data obtained by the groups of McGimsey (1975), Kikuchi (1973), Tabara (1974), and the Verons (1975). For the quasar 3C 345 and the BL Lacertae objects OJ 287 and BL Lac it is found that the optical flareup occurs first almost simultaneously in B and V and only later (about 8 days for BL Lac and OJ 287 and about 30 days for 3C 345) in U. This time sequence conforms to the predictions of the multiple supernova model of Colgate and his associates (1970) and of the multiple pulsar model of Arons, Kulsrud, and Ostriker (1975).

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