共查询到20条相似文献，搜索用时 31 毫秒
1.
Rapid flux density variations on timescales of the order of a day or less (Intraday Variability, IDV) in the radio regime are a common phenomenon within the blazar class. Observations with the Effelsberg 100-m telescope of the MPIfR showed that the variations occur not only in total intensity, but also in the polarized intensity and in polarization angle. Here we present an overview of our IDV-observations and discuss briefly some models which may explain the effect. 相似文献
2.
The results of a photometric monitoring of the quasar 4C 38.41, performed at the optical R and B bands in 2002 February–March, are presented. With a 60/90 cm Schmidt telescope at the Xinglong station of the National Astronomical Observatories of China, we observed the source exhibiting amplitude variations of up to 0.78 mag in both bands during the whole campaign. Intraday and even intranight variations are detected as well. A typical variability time-scale of about 36 d is derived from our 2-month observations at the optical bands, which is identical to that found at a radio wavelength of 92 cm, suggesting a common origin for the variations in 4C 38.41 from optical to radio bands. 相似文献
3.
Observational manifestations and intrinsic properties of the RCR sources in terms of a unified model
We present a summary results of the study of radio sources showing significant variations of integral flux density using the data from the RATAN-600 surveys of 1980–1994 at a frequency of 7.6 cm. The majority of the detected variable sources have flat radio spectra, although there are also all other spectrum types found. Point and compact sources predominate, although all known morphological structures are found in the sample. Variability is detected both in quasars and galaxies. Using the catalog data, we found brightness variations in the optical and/or infrared ranges for a half of host objects of radio sources. We analyzed the properties of nonvariable and variable RCR sources. We compared the ratio of absolute magnitude to radio luminosity for sources with the active nucleus types determined from the optical data. It is found that this parameter is approximately the same for quasars with different radio luminosity. It isminimum for the strongest radio galaxies and grows up to the level characteristic of quasars with the decrease of radio luminosity. Considering that the ratio depends on obscuring properties of a dust torus, such behavior can be explained if we assume that the torus geometry and its optical depth depend on the source long. This parameter is slightly higher among variable sources than among nonvariable ones which counts in favor of the nucleus more open to an observer. 相似文献
4.
An optical monitoring shows Blazar object S5 0716+714 has complex Intra-Day Variability (IDV) behaviour. In this paper, we introduce a method of non-linear time series analysis, and calculate the correlation dimension of the IDV light curves of S5 0716+714 over seven nights in the December of 2006. According to our calculations, the correlation dimension D ≈ 1.993 ? 5.178 for all of the observed data, it is implied that the IDV behaviour may be a chaotic system with some additional noise. 相似文献
5.
The possibility that BL Lac S5 0716+714 exhibits a linear root mean square (rms)-flux relation in its IntraDay Variability (IDV) is analysed. The results may be used as an argument in the existing debate regarding the source of optical IDV in Active Galactic Nuclei. 63 time series in different optical bands were used. A linear rms-flux relation at a confidence level higher than 65 % was recovered for less than 8 % of the cases. We were able to check if the magnitude is log-normally distributed for eight timeseries and found, with a confidence ≥95 %, that this is not the case. 相似文献
6.
P. L. Dufton F. P. Keenan D. Kilkenny D. O'Donoghue Q. A. Parker F. van Wyk & F. van Leeuwen 《Monthly notices of the Royal Astronomical Society》1998,297(2):565-569
International Ultraviolet Explorer low-resolution and optical moderate-resolution spectra are presented for the high galactic latitude β Cephei type star, PHL 346. Variability is identified in both the ultraviolet flux and the radial velocity with periods and phases consistent with those previously deduced from optical photometry. The similarity of both the flux and the radial velocity amplitude to those previously reported for the β Cephei variable, γ Pegasus, is striking and provides evidence for PHL 346 being a young core hydrogen burning star. A distance estimate for PHL 346 of approximately 7 kpc (corresponding to a z -distance of approximately 6 kpc) is obtained by scaling the distance of γ Pegasus obtained from Hipparcos observations. 相似文献
7.
Observations of the X-ray pulsar Vela X-1 with the ART-P telescope onboard the Granat Observatory are presented. Variability on a time scale of several thousand seconds was detected; intensity variations are shown to be accompanied by changes in the source’s spectrum. The hardness was also found to be highly variable on a scale of one pulsation period. The source’s spectrum exhibits an absorption feature at energy ～7 keV, which is apparently attributable to cyclotron scattering/absorption in the neutron-star magnetic field. Weak persistent emission was detected during an X-ray eclipse, which probably resulted from the scattering of pulsar emission in the stellar wind from an optical star. 相似文献
8.
Martin Haas Peter Biermann Rolf Chini Jochen Heidt Wolfram Kollatschny Helmut Meusinger Ralf Siebenmorgen 《Astronomische Nachrichten》2005,326(7):535-558
D01 Direct evidence of the receding ‘torus’ around active galactic nuclei of FRII radio galaxies and quasars D02 Infrared emission from a clumpy and dusty torus around AGN D03 Size and properties of AGN narrow–line regions from emission–line diagnostics D04 Structural Variability of Intraday Variable Sources D05 Stability of self‐gravitating accretion disks in galactic centers D06 Supermassive Binary Black Holes in AGN D07 The extreme flare in III Zw 2: Evolution of a radio jet in a Seyfert galaxy D08 Radio Linear and Circular Polarization from M81* D09 A fundamental relation between Supermassive Black Holes and Dark Matter Haloes D10 Hunting for radio‐quiet BL Lacs – the 2dF BL Lac survey D11 The Eddington limit in accretion discs D12 Molecular Tori in AGN: A search using excited states of OH D13 The X‐Ray Properties of Radio‐Loud Core‐Dominated AGN: The 2 cm‐X‐Sample D14 The X‐Ray Properties of Radio‐Loud Core‐Dominated AGN: Extension to the High Redshift Regime D15 Line Profile Variability in AGN D16 Jet Superwind Interaction D17 Radio Interferometric Observations of AGN – Probing the Nucleus of M87 with 20 Schwarzschild radii resolution D18 The ISO–2MASS AGN survey D19 Supermassive binary black holes driving the activity of galactic nuclei D20 Proton acceleration at quasi‐perpendicular shocks: A case study for Active Galactic Nuclei D21 Super‐luminal shocks in Active Galactic Nuclei D22 Unconventional quasars from the variability and proper motion survey D23 Radio observations of starburst and AGN activity in Ultraluminous Infrared Galaxies D24 Kinematics in Active Galactic Nuclei at Parsec Scales: the VLBA 2cm Survey D25 Three‐dimensional models of clumpy tori in Seyfert galaxies D26 Silicate emission in active galaxies ‐ From LINERs to QSOs D27 Discovery of 10 µm silicate emission in quasars. – Evidence of the AGN unification scheme. D28 Near‐IR adaptive optics imaging of luminous infrared galaxies D29 Interferometric observations of the Circinus galaxy with MIDI D30 Infrared Interferometry of the Seyfert Galaxy NGC 1068 相似文献
9.
Stefan J. Wagner 《Astrophysics and Space Science》2001,278(1-2):105-111
Intraday variability is detected in Blazars throughout the electromagnetic spectrum. Only radio emission is affected by interstellar
scintillation. The characteristics of variability observed at different frequencies are often similar and suggest that intrinsic
variations also contribute to the changes detected in the radio wavelength regime. This in turn implies very high brightness
temperatures. Unambiguous signatures of scintillation and of intrinsic changes have been identified. The properties of intrinsic
variations are reviewed to illustrate their potential contribution to variability in the radio domain. Such intrinsic changes
need to be discriminated against when studying scintillation in quasars and BL Lac objects. Observations of scintillating
sources and of sources with significant intrinsic IDV suggest interesting modifications to the standard paradigm of AGN.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
10.
V. L. Oknyansky N. V. Metlova O. G. Taranova V. I. Shenavrin B. P. Artamonov C. M. Gaskell 《Astronomy Letters》2014,40(9):527-536
We investigate the correlation between infrared (JHKL) and optical (B) fluxes of the variable nucleus of the Seyfert galaxy NGC4151 using partially published data for the last 6 years (2008–2013). We find that the lag of flux in all the infrared bands is the same, 40±6 days, to within the measurement accuracy. Variability in the J and K bands is not quite simultaneous, perhaps due to the differing contributions of the accretion disk in these bands. The lag found for the K band compared with the B band is not significantly different from earlier values obtained for the period 2000–2007. However, finding approximately the same lags in all IR bands for 2008–2013 differs from previous results at earlier epochs when the lag increased with increasing wavelength. Examples of almost the same lag in different IR bands are known for some other active nuclei. In the case of NGC 4151 it appears that the relative lags between the IR bands may be different in different years. The available data, unfortunately, do not allow us to investigate a possible change in the lags during the test interval. We discuss our results in the framework of the standard model where the variable infrared radiation is mainly due to thermal re-emission from the part of the dusty torus closest to the central source. There is also a contribution of some IR emission from the accretion disk, and this contribution increases with decreasing wavelength. 相似文献
11.
In the three years following the discovery of PSR J2051−0827, we have observed a large number of eclipse traverses over a wide frequency range. These data show that the pulsar usually undergoes complete eclipse at frequencies below 1 GHz. At higher frequencies the pulsar is often detected throughout this low-frequency eclipse region with pulse times of arrival being significantly delayed relative to the best-fitting timing model. Variability in the magnitude of the delay is clearly seen and occurs on time-scales shorter than the orbital period. Simultaneous dual frequency observations highlight the difference in the eclipse behaviour for two widely separated frequencies. The low-frequency eclipses are accompanied by a significant decrease in pulsed flux density, while the flux density variations during higher frequency eclipses are not well defined. We consider a number of eclipse mechanisms and find that scattering and cyclotron absorption in the magnetosphere of the companion are consistent with the phenomena presented here. 相似文献
12.
流星光学监测网是定位陨石和观测火流星的基础科研设施. 流星光学监测系统利用光学相机高速采集天空图像, 使用嵌入式系统实时处理数据, 能够快速识别流星并获取流星位置和陨石落点信息, 是构成流星监测网的关键仪器. 为提高流星光学监测系统获取信息的实时性及准确性, 提出了一种基于嵌入式人工智能设备的流星光学监测系统. 该系统由软件及硬件部分组成: 硬件部分包括观测设备(商用高空抛物摄像头)以及数据处理设备(嵌入式人工智能设备); 软件部分运行于数据处理设备内, 主要包括控制界面模块、流星监测模块、数据管理模块. 实际工作时, 摄像头采集天空视频信息, 流星监测模块从视频流中实时监测流星并存储包含流星视频的数据, 数据管理模块将流星位置信息实时传回数据中心用于预警. 观测结束后, 将原始观测数据同步至数据中心用于后续科学研究. 在整个系统中, 流星监测模块决定了整个监测系统的实时性及准确性. 该系统采用嵌入式人工智能设备与人工智能算法结合的方法构建流星监测模块. 通过使用实测数据对搭载监测模块性能进行测试, 结果表明: 流星监测模块能够达到0.28%的低误检率以及100%的召回率, 且数据处理速度达到了Mobilenetv2的8倍. 进一步将包含监测模块的整个流星光学监测系统部署于太原理工大学-张壁古堡远程天文台, 通过实测表明流星光学监测系统实用中能达到100%的召回率和较低的误检率. 相似文献
13.
Variability in 408-MHz flux density, over a 1-yr interval between 1995 and 1996, has been investigated using the DRAO Synthesis Telescope for a complete sample of 322 sources with S 408 MHz > 80 mJy at galactic latitude b = 15°; four sources are found to show significant flux density variations. These results, taken with those from a similar study at b = 58°, indicate that 408-MHz variability over a time-scale of 1 yr is more uncommon than has previously been thought; variations at a level >10 per cent could have been detected in a statistically complete sample of about 150 of these sources and none was found. Variability over a period of 18 yr has also been investigated by comparing the DRAO data with those from the B3 catalogue for 182 sources with S 408 MHz > 200 mJy; five variables are found. Large flux density variations over a period of 18 yr are much more common than over 1 yr, with roughly one source in 15 showing variations at the 15 per cent level or greater. The statistics are not good enough to show any conclusive evidence for a dependence of variability on galactic latitude. Roughly half of the variable sources have spectra that are steep at high frequencies and flatten at low frequencies; the other half have flat radio spectra over the entire frequency range. Simultaneous observations at 1420 MHz, also with the DRAO Synthesis Telescope, have been used to investigate variability at this frequency as well, and indicate that over a period of 1 yr roughly half of the flat-spectrum sources vary at the 5 per cent level or greater. 相似文献
14.
J. H. Fan Y. Liu Y. Li Q. F. Zhang J. Tao O. Kurtanidze 《Journal of Astrophysics and Astronomy》2011,32(1-2):67-71
Variability is one of the characteristics of blazars. The rapid variability is superposed on the long term variation. In this work, the variability on different time scales, such as intra-day (IDV), short-term (STV) and long-term (LTV) variations are presented for some sources. We also presented our own observations of some selected objects, for which the historical data were compiled for periodicity analysis using several methods. The parameters of the binary black hole system OJ 287 are determined. 相似文献
15.
16.
Wieslaw Z. Wisniewski 《Icarus》1976,28(1):87-90
Spectrophotometric and broad-band photoelectric observations of Eros are reported. No existing meteorite spectrum matches the asteroid data directly. Assemblages of iron or stony-iron with ordinary-chondrite material generate the best match for the reflectivity curve of Eros. Variability was found in the 0.6 micron band and V-R and V-I colors. 相似文献
17.
The blue-light observations of this pulsating and eclipsing variable (BCEP+EA) cover an interval from 1950 to 1992. The out-of-eclipse (that is, pulsational) variation contains three sinusoidal terms with variable amplitudes. In our 1996 paper (JP96), based on the 1950–1983 data, we showed that for the first two terms, having frequencies equal to about 5.9112 and 5.8551 d−1 , the amplitudes varied with time-scales of the order of 50 yr. The remaining term formed a doublet with constant amplitudes and frequencies close to 5.5033 d−1 , resulting in a beat-period of 1.85 yr. In the present paper we confirm this picture using additional data, derive improved values of the time-scales and refine the parameters of the doublet. In addition, we determine the year-to-year variation of the epochs of maximum light of the first two terms. This allows us to account for (1) the ground-based blue-filter observations that were not extensive enough to be used in the analysis, and (2) the Hp magnitudes from the Hipparcos mission. In particular, we demonstrate that the period of 0.171 203 d, given in the Hipparcos Variability Annex , is spurious. 相似文献
18.
S. Gburek M. Siarkowski A. Kepa J. Sylwester M. Kowalinski J. Bakala P. Podgorski Z. Kordylewski S. Plocieniak B. Sylwester W. Trzebinski S. Kuzin 《Solar System Research》2011,45(2):182-187
Solar Photometer in X-rays (SphinX) is an instrument designed to observe the Sun in X-rays in the energy range 0.85–15.00 keV. SphinX is incorporated within the Russian TESIS X and EUV telescope complex aboard the CORONAS-Photon satellite which was launched on January 30, 2009 at 13:30 UT from the Plesetsk Cosmodrome, northern Russia. Since February, 2009 SphinX has been measuring solar X-ray radiation nearly continuously. The principle of SphinX operation and the content of the instrument data archives is studied. Issues related to dissemination of SphinX calibration, data, repository mirrors locations, types of data and metadata are discussed. Variability of soft X-ray solar flux is studied using data collected by SphinX over entire mission duration. 相似文献
19.
We analyzed 134 images of Saturn taken by the Hubble Space Telescope between 1991 and 2004. The images cover wavelengths between 231 and 2370 nm in 30 filters. We combined some 10 million calibrated reflectivity measurements into 18,000 center-to-limb curves. We used the method of principal component analysis to find the main latitudinal and temporal variations in Saturn's atmosphere and their spectral characteristics. The first principal variation is a strong latitudinal variation of the aerosol optical depth in the upper troposphere. This structure shifts with Saturn's seasons, but the structure on small scales of latitude stays constant. The second principal variation is a variable optical depth of stratospheric aerosols. The optical depth is large at the poles and small at mid- and low latitudes with a steep gradient in-between. This structure remains essentially constant in time. The third principal variation is a variation in the tropospheric aerosol size, which has only shallow gradients with latitude, but large seasonal variations. Thus, aerosol sizes and their phase functions inferred at a particular season are not representative of Saturn's atmosphere at other seasons. Aerosols are largest in the summer and smallest in the winter. The fourth principal variation is a feature of the tropospheric aerosols with irregular latitudinal structure and fast variability, on the time scale of months. Spherical aerosols do not display the spectral characteristic of that feature. We suspect that variations in the shape of aerosols may play a role. We found a spectral feature of the imaginary index of aerosols, which darkens them near 400 nm wavelength. While we can describe Saturn's variations quite accurately, our presented model of Saturn's average atmosphere is still uncertain due to possible systematic offsets in methane absorption data and limitations of the knowledge about the shape of aerosols. In order to compare our results with those from comparable investigations, which used less than 30 filters, we fit models to spectral subsets of our data. We found very different best-fitting models, depending on the subset of filters, indicating a high sensitivity of results on the spectral sampling. 相似文献
20.
M. Wold M. S. Brotherton † Zhaohui Shang 《Monthly notices of the Royal Astronomical Society》2007,375(3):989-999
In order to investigate the dependence of quasar variability on fundamental physical parameters like black hole mass, we have matched quasars from the Quasar Equatorial Survey Team, Phase 1 (QUEST1) variability survey with broad-lined objects from the Sloan Digital Sky Survey. The matched sample contains ≈100 quasars, and the Sloan spectra are used to estimate black hole masses and bolometric luminosities. Variability amplitudes are measured from the QUEST1 light curves. We find that black hole mass correlates with several measures of the variability amplitude at the 99 per cent significance level or better. The correlation does not appear to be caused by obvious selection effects inherent to flux-limited quasar samples, host galaxy contamination or other well-known correlations between quasar variability and luminosity/redshift. We evaluate variability as a function of rest-frame time lag using structure functions and find further support for the variability–black hole mass correlation. The correlation is strongest for time lags of the order of a few months up to the QUEST1 maximum temporal resolution of ≈2 yr, and may provide important clues for understanding the long-standing problem of the origin of quasar optical variability. We discuss whether our result is a manifestation of a relation between characteristic variability time-scale and black hole mass, where the variability time-scale is typical for accretion disc thermal time-scales, but find little support for this. Our favoured explanation is that more massive black holes have larger variability amplitudes, and we highlight the need for larger samples with more complete temporal sampling to test the robustness of this result. 相似文献