天文学进展
天文學進展
천문학진전
PROGRESS IN ASTRONOMY
2009年
4期
358-372
,共15页
活动星系%耀变体%BL Lac
活動星繫%耀變體%BL Lac
활동성계%요변체%BL Lac
Astrophysics%active galaxies%individual blazers
耀变体在多个波段的微光变和能谱变化多年来是中外天文观测研究的热点课题.耀变体的微光变于20世纪60年代被发现,20世纪80年代以来发现很多源的微光变具有不同的特性,目前对其物理机制的认识和理论、模型的研究还处于发展阶段.该文总结了7个目前观测最多的耀变体(3C 66A,3C 279,3C 454.3,AO 0235+164,BL Lac,OJ 287,S5 0716+714)在光学波段的微光变和能谱变化的观测历史和最新进展,并对其理论模型作了简单介绍.
耀變體在多箇波段的微光變和能譜變化多年來是中外天文觀測研究的熱點課題.耀變體的微光變于20世紀60年代被髮現,20世紀80年代以來髮現很多源的微光變具有不同的特性,目前對其物理機製的認識和理論、模型的研究還處于髮展階段.該文總結瞭7箇目前觀測最多的耀變體(3C 66A,3C 279,3C 454.3,AO 0235+164,BL Lac,OJ 287,S5 0716+714)在光學波段的微光變和能譜變化的觀測歷史和最新進展,併對其理論模型作瞭簡單介紹.
요변체재다개파단적미광변화능보변화다년래시중외천문관측연구적열점과제.요변체적미광변우20세기60년대피발현,20세기80년대이래발현흔다원적미광변구유불동적특성,목전대기물리궤제적인식화이론、모형적연구환처우발전계단.해문총결료7개목전관측최다적요변체(3C 66A,3C 279,3C 454.3,AO 0235+164,BL Lac,OJ 287,S5 0716+714)재광학파단적미광변화능보변화적관측역사화최신진전,병대기이론모형작료간단개소.
Microvariability across the whole electromagnetic spectrum in blazars was first dis-covered in 1960s. It began to get extensive attention in 1980s. After twenty years' investigation,the physical mechanism leading to microvariability has not been found. Several models exist in explaining this phenomenon in the literature. The most widely accepted one is the shock-in-jet model. In this model, shocks propagating along the relativistic jet and interacting with the hydrodynamically turbulent plasma and twisted magnetic field should be responsible for the microvariability.Spectral variability is always found when a blazar shows variability in brightness in both short and long timescale. There are many different phenomena. Some blazars, generally flat spectrum radio quasars, become redder when brighter. Some (generally BL Lac objects) show the opposite trend-bluer when brighter. Some show no spectral variability at all. When blazars are in different states, they exhibit different behavior in spectral variability. As an example, in the outburst of OJ 287 in 1994, it showed no color change at all. However, in its 2005 outburst, it was observed to be bluer when brighter. Another example is S5 0716+714, it has been observed to be bluer when brighter, redder when brighter as well as show no spectral change with brightness.This paper provides a comprehensive review of the historical study of microvariability as well as spectral variability of seven most extensively observed blazars, namely 3C 279, 3C 454.3, 3C 66A, AO 0235+164, BL Lac, OJ 287, $5 0716+714. Models for these blazars' variability are also simply introduced.