共找到 20 条结果
BL Lac has been observed during the outburst occurred in the 1997 summer (Noble et al. 1997; Bloom et al. 1997) in three optical bands (BVI), with the aim of studying the intranight colour variations on very short timescales. Due to the high luminosity of the source we could perform quasi-simultaneous measurements in the three bands with a resolving time of about 5 minutes using one single telescope. We have detected several microvariability events occurring on timescales ranging from 30 min up to 3.5 hours. The magnitude changes had different amplitudes in the three bands being larger for shorter wavelenghts, and the source showed a marked trend to became bluer when brigther. There was no evidence of quasi-periodic oscillations in our multicolour light curves.
This report analyzes the I-band CCD photometry of Nova V1974 Cygni from the 1997 observational season. The analysis shows that both short-term modulations with periods 0.0813 and 0.085 days are still present in the light curve of the star. We confirmed the stability of the shorter period which is interpreted as the orbital period of the binary system. Its value, determined using the O-C residuals, is P_{orb}=0.08125873(23) days = 117.0126(3) min. The longer period, which appeared in the light curve in 1994, was decreasing until the beginning of 1995 but then started to increase quite rapidly. In October 1996 the value of the period was 122.67\pm0.02 min. Until the next observing run the period significantly decreased. Its value, determined from our observations performed in July 1997, was 121.87\pm0.12 min. This means that the rate of change of the period in 1996-1997 was as high as $\dot P \approx 10^{-6}$. Such a rapid change of the period requires a large amount of rotational kinetic energy, if we assume that a 122-min periodicity is the rotation period of a white dwarf. Thus the more probable explanation is the hypothesis is that the longer period including a superhump period i
The 100m world rankings of the 1997 outdoor track and field competition season are reviewed, subject to corrections for wind effects and atmospheric drag. The rankings and times are compared with those of 1996, and the improvements of each athlete over the course of a year are discussed. Additionally, the athletes' wind-corrected 50m and 60m splits from the 1997 IAAF World Championships are compared to the 1997 indoor world rankings over the same distances, as an attempt to predict possible performances for the coming 1998 indoor season.
There has been intense debate about the causes of the 1997-1998 El Nino. One side sees the obvious intense westerly wind events as the main cause for the exceptional heating in summer 1997, the other emphasizes slower oceanic processes. We present a quantitative analysis of all factors contributing to the onset of this El Nino. At six months' lead time the initial state contributes about 40% of the heating compared with an average year, and the wind about 50%. Compared with 1996, these contributions are 30% and 90% respectively. As westerly wind events are difficult to predict, this limited the predictability of the onset of this El Nino.
We present the optical (V, R, and I) photometry for BL Lacertae, which was observed from 1997 through 1999, with the 1.56-m telescope at the Shanghai astronomical observatory (SHAO). After the 1997 outburst, it dimmed to a low state and then brightened again. During the period JD 2450701 to JD 2450701.5, variations of 0.40mag, 0.27mag, and 0.21mag over a time scale of 100 minutes were found for V, R, and I bands, suggesting that the variations were decreasing with wavelength. The correlation between V, R, and I is also analyzed using the DCF (Discrete Correlation Function) method. This shows that the variability in the V, R, and I bands are correlated with no time delay longer than 0.2 day.
Here we report the discovery in the X-ray band of the first afterglow of a gamma-ray burst. It was detected and quickly positioned by the Beppo-SAX satellite on 1997 February 28 (GRB970228). The X-ray afterglow source was detected with the X-ray telescopes aboard the same satellite about eight hours after the burst and faded away in a few days with a power law decay function. The energetic content of the X-ray afterglow results to be a significant fraction of gamma-ray burst energetics. The Beppo-SAX detection and fast imaging of GRB970228 started a multiwavelength campaign that lead to the identification of a fading optical source in a position consistent with the X-ray source.
This report provides a summary and bibliography for the research activities at the Princeton University Observatory and Department of Astrophysical Sciences during the period July 1, 1997 to June 30, 1998.
This contribution to the XXVII Symposium on Multiparticle Dynamics held in Frascati, Italy, September, 1997 consists of the following subject matter: (1) Introductory generalities. (2) Brief mention of some of the contributions to the meeting. (3) More extended discussion of a few specialized topics. (4) Discussion of the FELIX initiative for a QCD detector at the LHC.
The gamma-ray burst of 1997 February 28 was localized using the arrival-time analysis method with the Ulysses, BeppoSAX, and WIND spacecraft. The result is a plus-or-minus 31.5 arcsec (3 sigma) wide annulus of possible arrival directions which intersects both the position of the burst determined independently by the SAX Wide Field Camera, and the position of a fading X-ray source detected by the SAX focussing X-ray telescopes, and reduces these source location areas by factors of 7 and 1.5 respectively. The combination of the annulus and the SAX locations, a 0.76 square arcminute error box, is consistent with that of an optical transient source and an extended object, possibly a galaxy. We also present the time history, peak flux, and fluence of this event, and derive a model-independent lower limit to the source distance of ~11000 AU.
A complex event observed in the radio pulses from the Crab pulsar in 1997 included echoes, a dispersive delay, and large changes in intensity. It is shown that these phenomena were due to refraction at the edge of a plasma cloud in the outer region of the Crab Nebula. Several similar events have been observed, although in less detail. It is suggested that the plasma cloud is in the form of filaments with diameter around 3 x 10^11m and electron density of order 10^4 cm-3
Highlights from the RXTE All Sky Monitor (ASM) during 1996 and 1997 are reviewed with particular attention to X-ray transients. The ASM has detected 117 sources. These include 12 recurrent transients and 10 new X-ray sources, some of which began their outbursts before the launch of RXTE. The majority of the outburst profiles are strikingly different from the classical form, with its fast rise and slow decay. Some of the light curves appear quasi-persistent, which suggests that they are associated with secular changes in the accretion rate from the donor star rather than with a cyclic instability in the accretion disk. The nature of the compact object is uncertain in many cases, but there is a likelihood that the majority of new sources are black hole systems, while the majority of recurrent transients contain neutron stars. There is a correlation between the gross shape of the energy spectrum, as seen in the ASM hardness ratio, HR2 (5-12 keV / 3-5 keV), and the accretion subclass. These data, with important contributions from SAX, CGRO, and Granat, provide a deeper probe of the X-ray sky than has been available previously. However, there are important systematic effects to be inves
We review the status of lattice calculations of the deep-inelastic structure functions of the nucleon. In addition, we present some results on the pion and rho structure functions.
The work is a comments on the article of V. G. Pal'chikov, Yu. L. Sokolov, and V. P. Yakovlev, devoted to the measurement of the Lamb shift in the hydrogen atom and published in Physica Scripta, 55 (1997) 33-40.
We present spectra of three M subdwarfs which are common proper motion companions to F or G subdwarfs of known metallicity. The assumption that the companions have the same composition allows us to test the Gizis (1997, AJ, 113, 806) M subdwarf classification system and its correspondence to metallicity. The results are in excellent agreement with the Gizis (1997) scale, thereby showing that the Allard & Hauschildt (1995, ApJ, 445, 433) Extended model atmospheres agree well in the 6200 -- 7400 Angstrom region for cool metal-poor stars. We also show that the results are consistent with the main sequences of globular clusters using the Reid (1997, AJ, 114, 161) distance scale.
In our Comment (G.E. Volovik and V.M. Yakovenko, Phys. Rev. Lett. 79 (1997) 3792) to the Letter by W. Apel and Yu.A. Bychkov (Phys. Rev. Lett. 78 (1997) 2188) we questioned the derivation of the Hopf term in the hydrodynamic action for the Skyrmion dynamics in QHE. Our main argument was that the description in terms of Euler angles used by Apel and Bychkov was potentially dangerous since these angles were ill-defined. The Reply (W. Apel and Yu.A. Bychkov, Phys. Rev. Lett. 79 (1997) 3792) to our Comment confirmed our apprehension.
In the wake of numerous injuries and Donovan Bailey's media-stamped "sub-par" 100m victory of 10.03s at the 1997 Canadian Track and Field Championships, a medal hope at the 1997 World Championships seems grim for the Olympic Champion and World Record holder. However, when one considers that the 10.03s was run into a hefty head-wind (-2.1 m/s), a simple correction for this effect can help to restore Canada's faith in their sprint hero -- not to mention rewrite the record books again.
We present in this Letter the first coordinated radio occultation measurements and ultraviolet observations of the inner corona below 5.5 Rs, obtained during the Galileo solar conjunction in January 1997, to establish the origin of the slow solar wind. Limits on the flow speed are derived from the Doppler dimming of the resonantly scattered componentof the oxygen 1032 A and 1037 A lines as measured with the UltraViolet Coronagraph Spectrometer (UVCS) on the Solar and Heliospheric Observatory (SOHO). White light images of the corona from the Large Angle Spectroscopic Coronagraph (LASCO) on SOHO taken simultaneously are used to place the Doppler radio scintillation and ultraviolet measurements in the context ofcoronal structures. These combined observations provide the first direct confirmation of the view recently proposed by Woo and Martin (1997) that the slow solar wind is associated with the axes, also known as stalks, of streamers. Furthermore, the ultraviolet observations also show how the fast solar wind is ubiquitous in the inner corona, and that a velocity shear between the fast and slow solar wind develops along the streamer stalks.
During remarkable flaring activity in 1997 Markarian 501 was the brightest source in the sky at TeV energies, outshining the Crab Nebula by a factor of up to 10. Periods of flaring activity each lasting a few days were observed simultaneously by several gamma ray telescopes. Contemporaneous multiwavelength observations in April 1997 show that a substantial fraction of the total AGN power is at TeV energies indicating that high energy processes dominate the energetics of this object. Rapid variability, on time scales of less than a day, and a flat spectrum extending up to at least 10 TeV characterize this object. Results of 1997 observations by 6 telescopes are summarized and some of the implications of these results are discussed.
The recent results (Pardo & Poretti 1997, A&A 324, 121; Poretti & Pardo 1997, A&A 324, 133) obtained on the frequency content of Double-Mode Cepheids light curves and the properties of their Fourier parameters are reviewed. Some points briefly discussed in previous papers (no third periodicity, methodological aspects on the true peaks detection, the action of the cross coupling terms and the impact on theoretical models) are described.
This is the summary of the working group on Goldstone Boson Production and Decay of the Chiral Dynamics Workshop in Mainz, September 1-5, 1997. For the production aspects we discuss $π^0$ and $η$ production in nucleon-nucleon collisions and the behaviour of hadrons in various sum rules. For the decays we present a discussion on various $K$, $η$ and $π$ decay channels. Other aspects discussed are a new treatment of meson-meson scattering, the light-by-light contribution to the muon anomalous magnetic moment and progress in various aspects of the $p^6$ generating functional in the mesonic sector.