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991.
The BL Lac-type object 3C 66A was observed at the Crimean Astrophysical Observatory during the international project OJ-94.
Observations were made over 10 nights from February through December 2003 at the Cassegrain focus of the 125-cm AZT-11 telescope
with a photopolarimeter capable of simultaneous measurements in the UBVRI bands. In the course of our measurements the brightness
of the object increased by more than 1 magnitude in all these bands. Its color indices varied and the degree of polarization
decreased from ∼16% in February to ∼3% at the end of our observations. In December 2003 a rapid change in the position angle
from 15° to 40° was noticed. The spectral energy distribution Fn is well described by a power law with a spectral index a (Fν ∝ ν
−α
. The increase in brightness was accompanied by a reduction in the spectral index. The most probable mechanism for the observed
changes in the brightness, degree of polarization, and spectral index may be a decrease in the magnetic field strength or
a change in its configuration owing to a increase in the chaotic component of the field.
__________
Translated from Astrofizika, Vol. 49, No. 1, pp. 41–59 (February 2006). 相似文献
992.
993.
We calculate the direction of the rotational angular momentum vector,M, of comet 19P/Borrelly based on rotational lightcurve data from 2000, groundbased imaging of the coma during the Deep Space
1encounter, and the basic near-nucleus coma morphology as revealed by the Deep Space 1 spacecraft. For the most likely direction,
we derivea family of solutions (with center at RA = 221°, Dec = -7°) if the direction of M is towards the sunward hemisphere during the Deep Space 1 encounter, whereas if the rotation is of opposite sense, the diametrically
opposite family of solutions (with center at RA = 41°, Dec = 7°) would result. We argue that the coma morphology in September
2001 is consistent with the nucleus being a principal axis rotator or one observationally indistinguishable from it. Therefore,
for all practical purposes, the direction of the rotational angular momentum vector coincides with the spin axis. We also
discuss why the determination of the spin axis direction based on observations from the last apparition is in disagreement
with the current result. 相似文献
994.
ICE, the electric field experiment on DEMETER 总被引:9,自引:0,他引:9
995.
Petr Zasche 《Astrophysics and Space Science》2005,296(1-4):127-130
Four eclipsing binaries, which show apparent changes of period, have been studied with respect to a possible presence of the
light–time effect. With a least squares method we calculated new light elements of these systems, the mass function of the
predicted third body, and its minimum mass. We discuss the probability of the presence of such bodies in terms of mass function,
changes in radial velocity and third light in solution of light curves. 相似文献
996.
997.
随着数字技术的发展,数字信号处理芯片的速度越来越快,这为高速数字滤波的实时实现提供了可能。简要阐述了数字滤波的原理,并对两种数字滤波的实现方法进行了分析;给出了数字滤波较模拟滤波的优势;介绍了数字滤波在射电天文测量中的各种应用。 相似文献
998.
R.H.D. Townsend R.J. Ivison Ian Smail A.W. Blain D.T. Frayer 《Monthly notices of the Royal Astronomical Society》2001,328(2):L19-L22
A numerical model of the Leonid stream is developed, based on an earlier model which has been applied to the Perseid stream. The results for this model are applied to the 2001 Leonid return. By examining the full three-dimensional dispersion of individual 'streamlets' released from the Leonid parent comet, 55P/Tempel–Tuttle, we have derived an estimate for the temporal change in spatial density of each trail. Using this result along with an estimate for the location of the centres for individual streamlets and fits to previous Leonid storm profiles, we estimate that the activity from the shower will be broad and relatively strong (zenithal hourly rates perhaps in excess of 1000). In particular, streamlets from the 1766 and 1799 ejections contribute to activity peaking near 10 and 12 ut on 2001 November 18, respectively. Additional older material from 1633, 1666 and 1699, as well as more recent ejections from 1866 and 1833, contributes to a much broader secondary maximum near 17.5 ut on November 18. Comparison with other published models of predicted Leonid activity in 2001 shows general agreement in terms of timing, but the models differ significantly in terms of the relative magnitude of the activity (which other models suggest will be larger). Significant anisotropy in the impact hazard exists for satellites in the geostationary belt, with those over western longitudes most likely to be affected. Integrated fluences for the 2001 Leonid return suggest a hazard of order one magnitude greater than occurred for the 1999 Leonid storm. 相似文献
999.
1000.
M. J. Hardcastle D. M. Worrall M. Birkinshaw R. A. Laing A. H. Bridle 《Monthly notices of the Royal Astronomical Society》2002,334(1):182-192
We have used a deep Chandra observation of the central regions of the twin-jet Fanaroff–Riley class I (FRI) radio galaxy 3C 31 to resolve the thermal X-ray emission in the central few kpc of the host galaxy, NGC 383, where the jets are thought to be decelerating rapidly. This allows us to make high-precision measurements of the density, temperature and pressure distributions in this region, and to show that the X-ray emitting gas in the centre of the galaxy has a cooling time of only 5×107 yr . In a companion paper, these measurements are used to place constraints on models of the jet dynamics.
A previously unknown one-sided X-ray jet in 3C 31, extending up to 8 arcsec from the nucleus, is detected and resolved. Its structure and steep X-ray spectrum are similar to those of X-ray jets known in other FRI sources, and we attribute the radiation to synchrotron emission from a high-energy population of electrons. In situ particle acceleration is required in the region of the jet where bulk deceleration is taking place.
We also present X-ray spectra and luminosities of the galaxies in the Arp 331 chain of which NGC 383 is a member. The spectrum and spatial properties of the nearby bright X-ray source 1E 0104+3153 are used to argue that the soft X-ray emission is mostly due to a foreground group of galaxies rather than to the background broad absorption-line quasar. 相似文献
A previously unknown one-sided X-ray jet in 3C 31, extending up to 8 arcsec from the nucleus, is detected and resolved. Its structure and steep X-ray spectrum are similar to those of X-ray jets known in other FRI sources, and we attribute the radiation to synchrotron emission from a high-energy population of electrons. In situ particle acceleration is required in the region of the jet where bulk deceleration is taking place.
We also present X-ray spectra and luminosities of the galaxies in the Arp 331 chain of which NGC 383 is a member. The spectrum and spatial properties of the nearby bright X-ray source 1E 0104+3153 are used to argue that the soft X-ray emission is mostly due to a foreground group of galaxies rather than to the background broad absorption-line quasar. 相似文献