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Post Info TOPIC: Comet P/2006 VW139
Blobrana


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RE: Comet P/2006 VW139
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Comet 288P is at Opposition (2.066 AU) on the 6th January 2018.



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Blobrana


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Comet 288P
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Comet 288P makes its closest approach to the Earth (2.233 AU) in the constellation Scorpius on the 2nd June 2015.



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Blobrana


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Comet 288P/(300163) 2006 VW139
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Comet 288P/(300163) 2006 VW139 is at Opposition (2.240 AU) in the constellation Scorpius on the 26th May 2015

Ephemeris

Date    TT    R. A. (2000) Decl.     Delta      r    Elong.  Phase   Mag
2015 05 25    16 11 25.0 -19 32 03   2.2421  3.2544   178.0     0.6  20.3
2015 05 26    16 10 33.6 -19 30 31   2.2400  3.2527   178.5     0.5  20.3
2015 05 27    16 09 42.1 -19 28 59   2.2382  3.2509   178.1     0.6  20.3
2015 05 28    16 08 50.6 -19 27 27   2.2367  3.2492   177.3     0.8  20.3
2015 05 29    16 07 59.2 -19 25 55   2.2355  3.2474   176.3     1.2  20.3
2015 05 30    16 07 07.8 -19 24 22   2.2345  3.2457   175.2     1.5  20.3
2015 05 31    16 06 16.5 -19 22 50   2.2339  3.2439   174.1     1.8  20.3
2015 06 01    16 05 25.4 -19 21 18   2.2335  3.2421   172.9     2.2  20.3
2015 06 02    16 04 34.5 -19 19 46   2.2334  3.2404   171.8     2.6  20.3
2015 06 03    16 03 43.9 -19 18 14   2.2336  3.2386   170.7     2.9  20.3
2015 06 04    16 02 53.5 -19 16 44   2.2341  3.2368   169.5     3.3  20.3
2015 06 05    16 02 03.5 -19 15 13   2.2349  3.2350   168.4     3.6  20.3
2015 06 06    16 01 14.0 -19 13 44   2.2359  3.2333   167.2     4.0  20.3
2015 06 07    16 00 24.8 -19 12 16   2.2372  3.2315   166.1     4.3  20.3
2015 06 08    15 59 36.2 -19 10 49   2.2388  3.2297   165.0     4.7  20.3
2015 06 09    15 58 48.0 -19 09 23   2.2407  3.2279   163.8     5.0  20.3
2015 06 10    15 58 00.5 -19 07 58   2.2428  3.2261   162.7     5.4  20.3


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Blobrana


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Comet 288P/Spacewatch
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Comet 288P/Spacewatch is at Opposition (2.664 AU) on the 27th March 2014

Ephemeris

Date    TT    R. A. (2000) Decl.     Delta      r     Elong.  Phase   Mag
2014 03 28    12 28 56.7 +01 35 47   2.6639  3.6598   175.5     1.2  20.9
2014 03 29    12 28 12.9 +01 40 21   2.6640  3.6597   175.1     1.3  20.9
2014 03 30    12 27 29.0 +01 44 53   2.6644  3.6596   174.5     1.5  20.9
2014 03 31    12 26 45.2 +01 49 23   2.6651  3.6596   173.7     1.7  20.9
2014 04 01    12 26 01.5 +01 53 50   2.6661  3.6595   172.8     2.0  20.9
2014 04 02    12 25 17.9 +01 58 14   2.6673  3.6594   171.8     2.2  20.9
2014 04 03    12 24 34.4 +02 02 36   2.6689  3.6593   170.8     2.5  20.9
2014 04 04    12 23 51.2 +02 06 54   2.6708  3.6592   169.7     2.8  21.0
2014 04 05    12 23 08.2 +02 11 09   2.6730  3.6591   168.7     3.1  21.0
2014 04 06    12 22 25.5 +02 15 20   2.6755  3.6590   167.6     3.4  21.0
2014 04 07    12 21 43.2 +02 19 27   2.6783  3.6589   166.5     3.7  21.0
2014 04 08    12 21 01.2 +02 23 30   2.6814  3.6588   165.4     4.0  21.0
2014 04 09    12 20 19.5 +02 27 28   2.6848  3.6587   164.2     4.3  21.0
2014 04 10    12 19 38.3 +02 31 23   2.6884  3.6586   163.1     4.6  21.0
2014 04 11    12 18 57.6 +02 35 12   2.6924  3.6584   162.0     4.9  21.0
2014 04 12    12 18 17.3 +02 38 57   2.6966  3.6583   160.9     5.2  21.0
2014 04 13    12 17 37.6 +02 42 37   2.7011  3.6582   159.7     5.4  21.0
2014 04 14    12 16 58.4 +02 46 11   2.7059  3.6580   158.6     5.7  21.0
2014 04 15    12 16 19.8 +02 49 40   2.7110  3.6579   157.5     6.0  21.0
2014 04 16    12 15 41.8 +02 53 04   2.7163  3.6577   156.4     6.3  21.0
2014 04 17    12 15 04.5 +02 56 22   2.7220  3.6576   155.2     6.6  21.0
2014 04 18    12 14 27.8 +02 59 34   2.7278  3.6574   154.1     6.9  21.0
2014 04 19    12 13 51.8 +03 02 40   2.7340  3.6573   153.0     7.2  21.0
2014 04 20    12 13 16.5 +03 05 40   2.7404  3.6571   151.9     7.4  21.0
2014 04 21    12 12 41.9 +03 08 34   2.7470  3.6569   150.8     7.7  21.0
2014 04 22    12 12 08.1 +03 11 22   2.7539  3.6568   149.7     8.0  21.0
2014 04 23    12 11 35.1 +03 14 04   2.7611  3.6566   148.6     8.2  21.0
2014 04 24    12 11 02.8 +03 16 38   2.7685  3.6564   147.5     8.5  21.0
2014 04 25    12 10 31.4 +03 19 07   2.7761  3.6562   146.4     8.8  21.0
2014 04 26    12 10 00.9 +03 21 28   2.7840  3.6560   145.3     9.0  21.0
2014 04 27    12 09 31.2 +03 23 43   2.7921  3.6558   144.2     9.3  21.0
2014 04 28    12 09 02.5 +03 25 51   2.8005  3.6556   143.1     9.5  21.1
2014 04 29    12 08 34.6 +03 27 52   2.8090  3.6554   142.0     9.8  21.1
2014 04 30    12 08 07.7 +03 29 46   2.8178  3.6552   140.9    10.0  21.1


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Blobrana


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Comet P/2006 VW139
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Title: Exploring the nature of new main-belt comets with the 10.4m GTC telescope: (300163) 2006 VW139
Authors: J. Licandro, F. Moreno, J. de León, G. P. Tozzi, L. M. Lara, A. Cabrera-Lavers

We aim to study the dust ejected by main-belt comet (MBC) (300163) 2006 VW139 to obtain information on the ejection mechanism and the spectral properties of the object, to see if they are compatible with those of "normal" comets.
Images in the g and r band and a low-resolution spectrum in the 0.35-0.9 micron region were obtained with the GTC telescope (La Palma, Spain). Images were analysed to produce a colour map and derive a lower limit of the absolute magnitude. A Monte Carlo (MC) scattering model was used to derive dust properties such as mass loss rates and ejection velocities as a function of time. The spectrum was compared to that of MBC 133P/Elst-Pizarro and used to search for CN emission.
The spectrum of 2006 VW139 is typical of a C-class asteroid, with a spectral slope S=0.5±1.0%/1000A. It is similar to the spectrum of 133P and other MBCs. No CN emission is detected. A CN production rate upper limit of 3.76e23 1/s is derived. The MBC present a narrow almost linear tail that extends up to 40.000 km in the anti-solar direction and more than 80.000 km in the direction of the object's orbital plane. The colour of the tail is slightly redder than the Sun (S=3 to 6%/1000A). The MC dust tail model derived the mass loss rates and ejection velocity as a function of time, and the results show that the activity onset occurs shortly after perihelion, and lasts about 100 days; the total ejected mass is about 2e6 kg.
The spectrum of VW139 suggests that it is not a "normal" comet. It is typical of the other observed MBCs. Even if no CN emission is detected, the more likely activation mechanism is water-ice sublimation. Like other well studied MBCs, VW139 is likely a primitive C-class asteroid that has a water-ice subsurface depth reservoir that has recently been exposed to sunlight or to temperatures that produce enough heat to sublime the ice.

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Blobrana


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Title: P/2006 VW139: A Main-Belt Comet Born in an Asteroid Collision?
Authors: Bojan Novakovic, Henry H. Hsieh, Alberto Cellino

In this paper we apply different methods to examine the possibility that a small group of 24 asteroids dynamically linked to main-belt comet P/2006 VW139, recently discovered by the Pan-STARRS1 survey telescope, shares a common physical origin. By applying the Hierarchical Clustering and Backward Integration methods, we find strong evidence that 11 of these asteroids form a sub-group which likely originated in a recent collision event, and that this group includes P/2006 VW139. The objects not found to be part of the 11-member sub-group, which we designate as the P/2006 VW139 family, were either found to be dynamically unstable, or these are likely interlopers which should be expected due to the close proximity of the Themis family. As we demonstrated, statistical significance of P/2006 VW139 family is >99 per cent. We determine the age of the family to be 7.5 ±0.3 Myr, and estimate the diameter of the parent body to be about 11 km. Results show that the family is produced by an impact which can be best characterised as a transition from catastrophic to cratering regime. The dynamical environment of this family is studied as well, including the identification of the most influential mean motion and secular resonances in the region. Our findings make P/2006 VW139 now the second main-belt comet to be dynamically associated with a young asteroid family, a fact with important implications for the origin and activation mechanism of such objects.

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Blobrana


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Title: Discovery of Main-Belt Comet P/2006 VW139 by Pan-STARRS1
Authors: Henry H. Hsieh, Bin Yang, Nader Haghighipour, Heather M. Kaluna, Alan Fitzsimmons, Larry Denneau, Bojan Novakovic, Robert Jedicke, Richard J. Wainscoat, James D. Armstrong, Samuel R. Duddy, Stephen C. Lowry, Chadwick A. Trujillo, Marco Micheli, Jacqueline V. Keane, Laurie Urban, Timm Riesen, Karen J. Meech, Shinsuke Abe, Yu-Chi Cheng, Wen-Ping Chen, Mikael Granvik, Tommy Grav, Wing-Huen Ip, Daisuke Kinoshíta, Jan Kleyna, Pedro Lacerda, Tim Lister, Andrea Milani, David J. Tholen, Peter Veres, Carey M. Lisse, Michael S. Kelley, Yanga R. Fernandez, Bhuwan C. Bhatt, Devendra K. Sahu, Nick Kaiser, K. C. Chambers, Klaus W. Hodapp, Eugene A. Magnier, Paul A. Price, John L. Tonry 


Main belt asteroid (300163) 2006 VW139 (later designated P/2006 VW139) was discovered to exhibit comet-like activity by the Pan-STARRS1 survey telescope using automated point-spread-function analyses performed by PS1's Moving Object Processing System. Deep follow-up observations show both a short (~ 10") antisolar dust tail and a longer (~ 60") dust trail aligned with the object's orbit plane, similar to the morphology observed for another main-belt comet, P/2010 R2 (La Sagra), and other well-established comets, implying the action of a long-lived, sublimation-driven emission event. Photometry showing the brightness of the near-nucleus coma remaining constant over ~ 30 days provides further evidence for this object's cometary nature, suggesting it is in fact a main-belt comet, and not a disrupted asteroid. A spectroscopic search for CN emission was unsuccessful, though we find an upper limit CN production rate of Q_CN < 1.3x10^24 mol/s, from which we infer a water production rate of Q_H2O < 10^26 mol/s. We also find an approximately linear optical spectral slope of 7.2%/1000A, similar to other cometary dust comae. Numerical simulations indicate that P/2006 VW139 is dynamically stable for > 100 Myr, while a search for a potential asteroid family around the object reveals a cluster of 24 asteroids within a cutoff distance of 68 m/s. At 70 m/s, this cluster merges with the Themis family, suggesting that it could be similar to the Beagle family to which another main-belt comet, 133P/Elst-Pizarro, belongs.

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Blobrana


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The apparent main belt asteroid (300163) 2006 VW139 was found to have a cometary nature by H. Hsieh, R. Wainscoat & D. Larry (PS1 telescope).

The orbital elements of the comet indicate a perihelion passage on the 18th July, 2011, at a distance of ~2.4 AU from the Sun, and an orbital period of ~ 5.33 years.

CBET 2920  (Subscription)



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