HaleBopp彗星的爆发活动

９９６ 年９ 月至１１ 月间,对ＨａｌｅＢｏｐｐ 彗星进行了照相和光电观测．给出观测结果,包括几次爆发和可能的爆发活动     

THREE EVENTS OF OUTBURST OF COMET HALE-BOPP

The results of photographic observations of Comet Hale-Bopp made at Qingdao Station of Purple Mountain Observatory during the period from September to November of 1996 are given. It is shown that three events of outburst occurred on Sept. 24, Oct. 26 and Nov. 13, and a large jet appeared in the plate of Sept.23,1996.     

Solar flare X-ray spectra

Spectra of 3 large flares on 24 Oct., 5 Nov. and 16 Nov. 1970 in the region = 1.75–1.95 Å, obtained with the help of the Intercosmos-4 satellite during solar activity maximum are given. The physical conditions at the initial and final (decaying) phases are mainly studied. The line spectra are compared with hard continuum in the region 8–80 keV and results of polarization measurements, obtained simultaneously aboard the same satellite.     

Spectroscopic observations of PU vulpeculae and its binary nature

The peculiar nova-like star PU Vul was observed spectroscopically from 1981 Sept 12 to 1983 Dec 11 at Yunnan Observatory and Beijing Observatory. In 1981 Sept, the star showed an absorption spectrum of the Balmer lines, the H,K and D lines, and some FeII, SrII and TiII lines. H was seen in emission in 1982 Oct and Hβ, in 1983 Sept. Both emissions were enhanced in 1983 Oct. and then dimmed since 1983 Nov. On 1983 Dec 11, Hβ might be absent, but the H was still visible. The spectral type was similar to that of an F giant during this period. This object may be an exceptionally slow nova and a binary consisting of an M giant and a hot companion.     

Sunspot numbers based on historic records in the 1610s: Early telescopic observations by Simon Marius and others

Hoyt & Schatten (1998) claim that Simon Marius would have observed the sun from 1617 Jun 7 to 1618 Dec 31 (Gregorian calendar) all days, except three short gaps in 1618, but would never have detected a sunspot – based on a quotation from Marius in Wolf (1857), but mis‐interpreted by Hoyt & Schatten. Marius himself specified in early 1619 that for one and a half year... rather few or more often no spots could be detected... which was never observed before (Marius 1619). The generic statement by Marius can be interpreted such that the active day fraction was below 0.5 (but not zero) from fall 1617 to spring 1619 and that it was 1 before fall 1617 (since August 1611). Hoyt & Schatten cite Zinner (1952), who referred to Zinner (1942), where observing dates by Marius since 1611 are given but which were not used by Hoyt & Schatten. We present all relevant texts from Marius where he clearly stated that he observed many spots in different form on and since 1611 Aug 3 (Julian) = Aug 13 (Greg.) (on the first day together with Ahasverus Schmidnerus); 14 spots on 1612 May 30 (Julian) = Jun 9 (Greg.), which is consistent with drawings by Galilei and Jungius for that day, the latter is shown here for the first time; at least one spot on 1611 Oct 3 and/or 11 (Julian), i.e. Oct 13 and/or 21 (Greg.), when he changed his sunspot observing technique; he also mentioned that he has drawn sunspots for 1611 Nov 17 (Julian) = Nov 27 (Greg.); in addition to those clearly datable detections, there is evidence in the texts for regular observations. For all the information that can be compared to other observers, the data from Marius could be confirmed, so that his texts are highly credible. We also correct several shortcomings or apparent errors in the database by Hoyt & Schatten (1998) regarding 1612 (Harriot), 1615 (Saxonius, Tard´e), 1616 (Tard´e), 1617–1619 (Marius, Riccioli/Argoli), and Malapert (for 1618, 1620, and 1621). Furthermore, Schmidnerus, Cysat, David & Johann Fabricius, Tanner, Perovius, Argoli, and Wely are not mentioned as observers for 1611, 1612, 1618, 1620, and 1621 in Hoyt & Schatten. Marius and Schmidnerus are among the earliest datable telescopic sunspot observers (1611 Aug 3, Julian), namely after Harriot, the two Fabricius (father and son), Scheiner, and Cysat. Sunspots records by Malapert from 1618 to 1621 show that the last low‐latitude spot was seen in Dec 1620, while the first high‐latitude spots were noticed in June and Oct 1620, so that the Schwabe cycle turnover (minimum) took place around that time, which is also consistent with the sunspot trend mentioned by Marius and with naked‐eye spots and likely true aurorae. We consider discrepancies in the Hoyt & Schatten (1998) systematics, we compile the active day fractions for the 1610s, and we critically discuss very recent publications on Marius which include the following Maunder Minimum. Our work should be seen as a call to go back to the historical sources. (© 2016 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

NOAA6361活动区现象分析

本文分析了ＮＯＡＡ６３６１活动区中的一些现象，发现该活动区在衰亡阶段经历了两次同极性黑子的复合过程，复合后的黑子本影间均有光桥存在，观测结果倾向于支持Ｐａｒｋｅｒ１９７９年提出的黑子多磁流管模型。１４日复合后的黑子本影还顺时针方向旋转了约７０度角，从半影纤维的同样顺时针旋转可以认为：该黑子的半影磁场并非是普遍认为的简单的本影磁场的发散部分。我们还观测到另外两个比较有趣的现象：①δ黑子中的ｐ极性黑子     

地球大气边界层结构和天文视宁度

依据声雷达资料和其他边界层资料讨论了大气边界层结构、地形等对视宁度的影响和有关选址问题．     

The semi-detached binary system RZ draconis

The 1978 photoeletric observations of the late type close binary RZ Dra were reanalyzed with the Wilson and Devinney approach. Photometric parameters were determined (in Tab. 1.). The system is found to be semi-detached where the less massive component fills its Roche surface, whereas the other component almost does so. The configuration of the system is shown in Fig. 1. The absolute dimensions of the system are found to be M₁ = 0.61M⊙, $\text{M}{}_2\text{= 0.41}\text{M}\text{⊙}\text{R}{}_1\text{= 1.15}\text{R}\text{,}\text{?}\text{and}\text{R}{}_2\text{= 0.96}\text{R}\text{⊙}$. Both components appear to be overluminous and oversized for their masses and spectral types. Its evolutionary stage is also discussed. The variability in the brightness of the primary mlnimum(Fig. 4) indicates mass loss from the vicinity of L₂, which would be mainly responsible for the long-term decrease in its period.     

Beobachtungen Kleiner Planeten. XIII

Es wird eine Übersicht gegeben über die im Jahr 1992 auf Tautenburger Schmidtplatten gefundenen Kleinen Planeten. Es wurden 518 Objekte beobachtet und für diese 2396 Positionen gerechnet. Es handelt sich um 408 Planetoiden mit provisorischer Bezeichnung, unter denen 274 neu vergebene Bezeichnungen sind, sowie um 110 numerierte Objekte. Für 172 Tautenburger Objekte wurden Bahnen aus einer Opposition gerechnet. Für 55 im Berichtszeitraum numerierte Planeten haben Tautenburger Positionen einen Beitrag geleistet. Acht Tautenburger Planetoiden wurden numeriert (Tab. 3). A summary is given about the Minor Planet survey performed in 1992 on Tautenburg Schmidt plates. 518 asteroids were observed and 2396 positions are calculated for them. These are 408 asteroids with provisional designations (274 of them have new designations) and 110 numbered objects. One-opposition orbits have been computed for 172 Tautenburg asteroids. Tautenburg observations could give a contribution to 55 planets numbered in the period of this report. Eight Tautenburg asteroids have been numbered (Tab. 3).     

A dynamical model with a new inversion technique applied to observations of Comet C/2000 WM1 (LINEAR)

Three continuum images of Comet C/2000 WM₁ (LINEAR) obtained on Nov 10, Nov 19, and Dec 03, 2001, are analyzed with the aid of a dynamical model, i.e. with a model that uses the size-dependent motion of dust grains under solar radiation pressure to determine the dust size distribution and its temporal change. The frames are photometrically calibrated in terms of the albedo filling factor product. On Nov 20.2 the Earth transited the orbital plane of the comet and an anti-tail was recognized in the image of Nov 19. For the determination of the particle fluxes describing the contribution of monodisperse particle shells to the cometary brightness the model uses a new regularization method employing Chebyshev polynomials of selected orders in emission time and particle size. It guarantees positiveness of the particle fluxes and imposes a varying degree of smoothness on their dependence on particle size and emission time. The particle emission velocities are still derived by trial and error. The dynamical model is described in detail. Results are presented for several low orders of the Chebyshev polynomials and are compared in order to understand the limitations imposed by the regularization process. The size distributions derived from the different observations do not always agree. This is particularly true for the earliest and most recent synchrones contributing to an image. In the observations of Nov 10 and Dec 03, i.e. excluding the anti-tail image, the integrated mass loss strongly decreases in the most recent time steps of the model although the comet is still approaching the Sun. This is interpreted as an artifact introduced by the overlap of the shells of large particle size emitted shortly before the observation. The model derives an increasing number of small particles released by the comet in the second half of November. This is at least in part considered as real and attributed to particle fragmentation occurring when the comet was at a heliocentric distance of about 1.4 AU.     

Beobachtungen Kleiner Planeten. XIV

A summary is given about the Minor Planet survey performed in 1993 on Tautenburg Schmidt plates. 392 asteroids were observed and 1462 positions are calculated for them. These are 297 asteroids with provisional designations (217 of them have new designations) and 95 numbered objects. Ten new designations originate from the KSO-ARI-Survey IV. Tautenburg observations could give a tribute to 50 planets numbered in the period of this report. Six Tautenburg asteroids have been numbered (Tab. 3).     

A possible rotation period for the minor planet 164 Eva

The minor planet 164 Eva passed through opposition on December 1, 1975 with a magnitude B_opp = 11.3 mag. Photoelectric observations at the Observatory of Torino, Italy, were carried out in two nights on Oct. 27/28 and Nov. 11, each with a run of about 3 hr. Two further successful photoelectric observations were carried out at the OHP, France, each with a run of about 6 hr. From all observed parts of the lightcurve a resulting synodic period of rotation of about 27.3 hr can be deduced, with a range of the total amplitude of at least Δm = 0.07 mag. With this period of 27.3 hr the minor planet 164 Eva is one more long period object, falling now between 654 Zelinda (H. J. Schober, 1975, Astron. Astrophys.44, 85–89) and 139 Juewa (J. Goguen et al., 1976, Icarus29, 137–142), at the high end in the histogram of the distribution of minor planet rotation periods.     

1998年德令哈狮子座流星雨目视观测及初步分析

根据中国－荷兰狮子座流星雨合观测1998年11月13日至18是日在紫金山天文台德令哈观测站观测所得的数据，以及同期中国其他地方的观测数据，分析了1998年狮子座流星雨的分布特征，提出此次地球所遭遇的流星群带呈3层结构。     

Beobachtungen Kleiner Planeten. XII

Es wird eine Übersicht gegeben über die im Jahr 1991 auf Tautenburger Schmidtplatten gefundenen Kleinen Planeten. Es wurden 533 Objekte beobachtet und für diese 2066 Positionen gerechnet. Es handelt sich um 456 Planetoiden mit provisorischer Bezeichnung, unter denen 324 neu vergebene Bezeichnungen sind, sowie um 77 numerierte Objekte. Für Tautenburger Objekte wurden 250 Bahnen aus einer Opposition gerechnet. Für 54 im Berichtszeitraum numerierte Planeten, darunter befinden sich auch (4999) MPC und (5000) IAU, haben Tautenburger Positionen einen Beitrag geleistet. Neun Tautenburger Planetoiden wurden numeriert (Tab. 3). A summary is given about the Minor Planet survey performed in 1991 on Tautenburg Schmidt plates. 533 asteroids were observed and 2066 positions are calculated for them. These are 456 asteroids with provisional designations (324 of them have new designations) and 77 numbered objects. One-opposition orbits have been computed for 250 Teutenburg asteroids. Tautenburg observations could give a tribute to 54 planets numbered in the period of this report, among them are (4999) MPC and (5000) IAU, too. Nine Tautenburg asteroids have been numbered (Tab. 3).     

X级耀斑过程中的磁剪切变化(英文)

通过对活动区NOAA 6891中三个X级耀斑前后的向量磁场分析 ,研究耀斑发生条件与耀斑发生前后横向磁场和磁剪切变化的关系。我们发现与Hagyard的耀斑发生条件不同的是 ,强的横向磁场和磁剪切不是活动区中耀斑发生的充要条件。我们的结果表明 ,活动区NOAA 6891 1 991年 30日的耀斑发生在横向磁场和磁剪切剧烈下降后。尽管 1 0月 2 7日的耀斑发生后横向磁场和磁剪切变化很大 ,但由于有新磁流浮现 ,造成磁中性线的改变 ,使得横向磁场和磁剪切变化与耀斑发生的联系变得比较复杂。     

带食而出的天光变化

作为“夏商周断代工程．天再旦”研究的一部分,讨论带食而出的天光变化．用照相机测光的方法测定正常日出前后的天光变化规律,建立带食而出的天光视亮度变化计算方法,并给出计算“天再旦”现象的范围和强度的方法．为此于1997年3月9日在新疆组织了群众性的日食观测．实测证实带食而出的确可以引起“天再旦”现象,同时与理论计算有很好的符合.     

电离层对GPS测距的影响

利用单层电离层改正模型就GPS卫星高度角对测距的影响作了探讨。研究表明，通常采用的单层电离层改正模型中电离层高取均值对低高度角卫星测距的改正是不适应的，利用单层电离层模型改正时应顾及电离层高的变化。最后利用1986年武汉地区实测TEC数据进行了计算并将结果和IRI－90模型计算结果作了分析比较。     

太阳大气中双拱结构的平衡与非平衡

导出了非线性静磁平衡方程的一个幂级数形式的相似解,和使这一级数收敛的解的参数范围。阐明了在此范围内的一组参数对应于一个平衡位形和在这个范围之外的一组参数不对应于一个平衡位形(非平衡)。并绘出了一个非线性的平衡位形。 结果可用于解释:多带耀斑的产生、双拱磁结构和拉长的复杂黑子群上空的磁场结构。     

北京天文台60cm望远镜的新光电光度计

本文介绍了北京天文台新研制的光电光度计。本光度计是带有微计算机星天交替式的。可通过计算机控制实现星天和滤光片自动转换。可以很方便地进行随机采集和连续采集,可以实时显示数据和处理观测结果。已经正规观测两年多,取得了一批观测成果,精度可达±0.003~m,能很好地归化到国际系统。     

Observational effect for the lunar gravity on meteor streams

Meteoroids always posed a great hazard to spacecraft security. A meteoroids stream assembled by a large massive body will further enhance the hazard severalfold. For example, the radiant of Northern Taurids (NTA) will be occulted by the Moon on Nov. 12, 2011. Since the gravitational lensing effect of massive bodies can gather together the orbits of meteoroids, the observable flux of meteoroids will increase. In this paper a set of numerical methods was built to discuss the observational effect of this kind of phenomena. The ZHR of NTA is generally small. But it can be local strong on the Earth by the lunar gravitational assembling. The calculated result suggests that a ten times stronger than normal NTA will appear in the sea area of Tristan da Cunha islands during 00h45m UT to 02h00m UT on Nov. 12, 2011.