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Post Info TOPIC: Comet 73P/Schwassmann-Wachmann 3


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Comet 73P/Schwassmann-Wachmann 3-Y
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Comet 73P/Schwassmann-Wachmann 3-Y makes its closest approach to the Earth (1.558 AU) on the 19th March 2018.



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Comet 73P/Schwassmann-Wachmann 3-T
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Comet 73P/Schwassmann-Wachmann 3-T will make its closest approach to the Earth (1.276 AU) on the 1st March 2018.



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RE: Comet 73P/Schwassmann-Wachmann 3
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Comet 73P/Schwassmann-Wachmann is at Opposition (4.069 AU) on the 11th December 2013

 



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Comet 73P-C/Schwassmann-Wachmann C makes its closest approach to the Earth (1.595 AU) on the 4th November, 2011.

Google earth file: Comet 73P-CSchwassmann-Wachmann C.kmz (18kb, kmz)



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Comet 73P-C/Schwassmann-Wachmann C
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Comet 73P-C/Schwassmann-Wachmann C is at Perihelion (0.943 AU) on the 16th October, 2011.



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Comet 73P/Schwassmann-Wachmann 3B
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Title: 2006 Fragmentation of Comet 73P/Schwassmann-Wachmann 3B Observed with Subaru/Suprime-Cam
Authors: Masateru Ishiguro, Fumihiko Usui, Yuki Sarugaku, Munetaka Ueno

We analysed the Subaru/Suprime-Cam images of 73P/Schwassmann-Wachmann 3B and detected no fewer than 154 mini-comets. We applied synchrone-syndyne analysis, modified for rocket effect analysis, to the mini-fragment spatial distribution. We found that most of these mini-comets were ejected from fragment B by an outburst occurring around 1 April 2006. The ratio of the rocket force to solar gravity was 7 to 23 times larger than that exerted on fragment B. No significant colour variation was found. We examined the surface brightness profiles of all detected fragments and estimated the sizes of 154 fragments. We found that the radius of these mini-fragments was in the 5- to 108-m range (equivalent size of Tunguska impactor). The power-law index of the differential size distribution was q = -3.34 ±0.05. Based on this size distribution, we found that about 1-10% of the mass of fragment B was lost in the April 2006 outbursts. Modelling the cometary fragment dynamics revealed that it is likely that mini-fragments smaller than ~10-20 m could be depleted in water ice and become inactive, implying that decameter-sized comet fragments could survive against melting and remain as near-Earth objects. We attempted to detect the dust trail, which was clearly found in infrared wavelengths by Spitzer. No brightness enhancement brighter than 30.0 mag arcsec^-2 (3sigma) was detected in the orbit of fragment B.

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RE: Comet 73P/Schwassmann-Wachmann 3
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Title: OCCULTATION OBSERVATION TO PROBE THE TURBULENCE SCALE SIZE IN THE PLASMA TAIL OF COMET SCHWASSMANN-WACHMANN 3-B
Authors: NIRUPAM ROY1 , P. K. MANOHARAN2, AND PAVAN CHAKRABORTY3

We present the occultation observation of compact radio source B0019000 through the plasma tail of comet Schwassmann-Wachmann 3-B. The observation was made with the Ooty Radio Telescope at 326.5 MHz on May 26, 2006 when the plasma tail of the comet was in front of this source.
 The scintillation was found to be increased significantly for the target source compared to that of a control source. The intensity fluctuation power spectra show both steepening at high spatial scales and excess power at low spatial scales. This observation can be attributed to the turbulence in the comet plasma tail. A two-regime plasma turbulence can explain the time-evolution of the power spectrum during the occultation observation.

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Animation of 73/P Schassmann-Wachmann on  5. April 2006



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A well-studied comet appears to be uniform in chemical composition. Scientists from Johns Hopkins University and LESIA of Paris Observatory studied two fragments from the disintegrating comet 73P/Schwassmann-Wachmann 3. The fragments reveal a range of different depths, and they were found very similar in icy composition. This goes against the theory that outer layers of comet nuclei are heavily processed by solar radiation, making their outsides chemically different to their insides.
The composition of cometary ices provides key information on the chemical and physical properties of the outer solar nebula where comets formed, 4.6 Gy ago. About two dozen molecules released from the sublimation of nucleus ices have been identified in cometary atmospheres, mainly by infrared and microwave spectroscopy. Chemical diversity is observed both in the class of Oort cloud comets and within the Jupiter-family comet population consisting of short-period comets formed in the Kuiper belt. This remarkable diversity can be attributed to several factors including differences in the chemical and physical environments in comet-forming regions, chemical evolution during their long storage in the Oort cloud and Kuiper belt, and thermal processing by the Sun when entering the inner Solar System. This latter mechanism, which may deplete the outer layers of comet nuclei in the most volatile species, is invoked to explain the low CO abundances measured in Jupiter-family comets, while several Oort cloud comets exhibit high CO abundances.

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Comets may have a more consistent mix of chemicals than previously thought, according to a new study that contradicts assumptions about the fiery celestial bodies.
Ground-based observations of two fragments from the nucleus of a comet called SW 3 indicate a "very homogeneous" composition, said study lead author Neil Dello Russo of Johns Hopkins University Applied Physics Lab in Maryland.

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