SL9彗星撞击木星时S碎片的CCD观测

用上海天台１．５６ｍ望远镜和ＣＣＤ照相机，观测Ｓ＝５碎片时，发现了类似彗尾的奇异现象。     

SL9彗星撞击木星时S碎片的CCD观测

用上海天文台１．５６ｍ望远镜和ＣＣＤ照相机，观测ｓ＝５碎片时，发现了类似彗尾的奇异现象。     

SL—9彗星六块碎片撞击时间的测定

在SL－9彗星撞击木星期间，用上海天台佘山观测站的1.56m望远镜和CCD照相机，观测木星卫星在接击期间的亮度变化，由此测定了六块碎片的撞击时间。     

苏梅克－利维9号彗星撞击木星事件的光学观测

本文给出了１９９４年７月１７日至２２日，彗星碰撞期间，福州和乌鲁木齐两个观测点所取得的部分光学观测资料。     

我国对苏梅克—列维9号彗星撞击木星事件的观测

１９９４年７月１６日－２２日，苏梅克－列维９号周期彗星的２１颗碎片连续撞击木星事件是一次极为罕见的天文现象。文中概括介绍了我国天文学家对彗木相撞事件的光学和射电观测网点、课题设置以及所取得的主要观测结果。     

1994年4月的SL9彗星观测

１９９４年４月１２日晨，我们对Ｓ９彗星进行了成功的观测．观测使用云南天文台一米望远镜和加了缩焦器的Ⅱ号ＣＣＤ系统．照相机像素为５１２×５１２，视场约７’×７’．在近两小时的不同时刻的四张照片中，观测到了彗星２１颗碎核中的主要部份及其运动．本文介绍了此次观测情况和资料处理，并给出对ＳＬ９各彗核的位置和亮度的测量结果．     

苏梅克—利维9号彗星撞击木星事件的光学观测

本文给出了１９９４年７月１７日至２２日，彗星碰撞期间，福州和乌鲁木齐两个观测点所取得的部分光学观测材料。     

木星大气探秘

仰望夜空观察木星,其亮度仅次于太阳、月球和金星（有的时候,木星会比火星稍暗,但有时却要比金星还要亮）。木星在太阳系的八颗行星中体积和质量堪称最大,以此有行星王子之称。     

击中木星——苏海克-列维9号彗星15年后

澳大利亚天文爱好者安东尼·韦斯利（Anthony Wesley）是一个非常热爱天空和细心的人。2009年7月19日晚11点,他打开了自己的37厘米口径望远镜观测木星（见图1）。天气状况并不十分令人满意。子夜刚过,视宁度更加恶化。他都准备收摊了,突然改变了主意,决定过半小时以后再来看看。大约12点40分,     

我国对苏梅克-列维9号慧星撞击木星事件的观测(英)

1994年7月16日─22日，苏梅克－列维9号周期慧星的21颗碎片连续撞击木星事件是一次极为罕见的天文现象．文中概括介绍了我国天文学家对慧木相撞事件的光学和射电观测网点、课题设置以及所取得的主要观测结果．     

1．56m望远镜观测彗－木相撞概况

用上海天文台佘山观测站的１．５６ｍ望远镜和ＣＣＤ照相机，观测到彗－木碰撞的六次事件。本文给出由撞击引起的木卫闪光Ｋ＝１２的光变曲线和一些碰撞后木星的照片。     

The impact of comet SL9 with Jupiter: IR observations at TIRGO

Infrared images of Jupiter have been obtained on 5 nights before, during and shortly after the period of the impacts of the fragments of comet Shoemaker-Levy 9 (1993e) with the giant planet. Long lived bright spots produced by the impacts have been measured and analyzed. By measuring the intensity variation of the spots as a function of Jupiter rotation we show that these spots are likely constituted by large and thin clouds of dust located above the methane layer. The IR relative albedos has been also measured for some of these spots.On leave from Center for Astrophysics - Cambridge (USA)     

Flux monitoring at 327 MHz during SL9-Jupiter collision

Jupiter flux at 327 MHz was monitored using the Ooty radio telescope from July 12th to July 29th during the collision of comet Shoemaker-Levi 9 with Jupiter. Flux was found to increase steadily from July 17th to July 26th by ∼ 2–5 Jy, after which it declined to its pre-event value. The comparison of 327 MHz observations with those at 840 MHz and 2240 MHz indicates that the enhancement was mainly due to the increased synchrotron emission and the contribution of thermal emission was very small at metric-decimetric frequencies. The enhancement in radio emission was found to be more at 840 MHz than at 327 or 2240 MHz. The steepening of the spectrum between 327 and 840 MHz as well as between 2240 and 840 MHz was also noted.     

THE FRAGMENTS OF COMET HYAKUTAKE (C/1996 B2)

Several fragments of Comet Hyakutake were observed in March and April of 1996. This leads to the impression that the splitting of Comet Hyakutake on a small scale occurred frequently. Data analysis points to a rotation period of about 6.18hr if the fragments of Apr. 11 are the condensations within a jet.     

Sodium emission from Comet Shoemaker-Levy 9 in the magnetosphere of Jupiter

On July 20, 1994, before the Q fragments of Comet Shoemaker-Levy 9 fell to Jupiter, more than 200 spectra of the Jovian features were obtained at the Crimean Astrophysical Observatory in the wavelength range 5700–7600 Å with a 26 s exposure time and a spectral resolution of 20 Å. We found a time-varying Na D line emission in the form of two components with Doppler shifts of about 30 Å. The brightest and most frequent sodium flares were detected when the Q fragments passed through the Jovian inner magnetosphere at a distance of about three the Jovian radii (3R_J) from its center, where they crossed the Io-Jupiter current tube. A frequency analysis of our data revealed a flare recurrence time scale of 1 min. We conclude that sodium was released from the cometary dust and from the surfaces of numerous cometary debris and that its amount was enough to produce the observed emission. The observed high-speed clouds of sodium atoms are assumed to have been formed through ionization, ion acceleration by the bidirectional electric fields of Alfvén waves in the Io-Jupiter current tube, and their neutralization.     

Optical imaging of impact sites of Comet Shoemaker-Levy 9 at Bisei Astronomical Observatory

The impact sites of the Comet Shoemaker-Levy 9 are observed with the 101-cm telescope at Bisei Astronomical Observatory until the end of August with B, V, R, I, and methane-band (0.89m) filters. The outline of the observation is briefly described.     

海尔—波普彗星自转周期的测定

采用小波方法对海尔波普彗星的近核ＣＣＤ图像进行处理,并进一步分析了彗核的亮度中心周围的特征结构,从而提出了一种直观而有效的方法来测定海尔波普彗星投射在观测平面上的平均自转周期,结果为２４．４１±０．９６小时