Comet Observation database (COBS) was developed in 2010 and is maintained by Crni Vrh Observatory. It is a unique service offering comet observers to submit, display and analyse comet data in a single location and is opened to comet observers worldwide. Registered observers may submit the observations using a simple web-based form which will store their observations into an SQL database and display them in ICQ format.
Data stored in COBS database is freely available to everyone with respect to our data usage policy, and can be analysed with COBS online tools or exported and further used in other analysis software and publications.
Database currently contains more than 226000 comet observations of more than 1200 different comets and represents the largest available database of comet observations.
Amateur comet observers can make a useful contribution to science by observing comets and submitting their observations to the COBS, as the professional astronomers do not have the time nor the telescopes needed to gather such data. We encourage comet observers worldwide to submit their observations and contribute to the COBS database.
Type Comet name Obs date Mag Dia DC Tail Observer V 2016U1 2016 12 06.19 10.5 4 1 BUIaa V 2015V2 2016 12 06.03 12.7 0.8 4 NOV01 V 2016U1 2016 12 06.02 11.0: 4 1 NOV01 C 2016U1 2016 12 06.00 10.9 6 1/ NOV01 C 2015V2 2016 12 05.96 13.0 1 4/ 1.2m316 NOV01 C 2016U1 2016 12 05.50 11.7 > 3.6 RAMaa C 2011KP36 2016 12 05.21 14.1 1.4 RAMaa V 2015V2 2016 12 05.18 12.0 1.5 3/ MEY V 2016U1 2016 12 05.17 10.4 4 1/ MEY V 2016U1 2016 12 04.49 10.5 3 1 HER02 V 45 2016 12 04.43 11.1 1.5 3 WYA V 2015V2 2016 12 03.21 12.2 1 4 0.02 KUT V 2016U1 2016 12 03.17 12.4 2.2 3 KUT V 2016U1 2016 12 03.15 10.7 3 1 HAR11 V 2015V2 2016 12 03.14 12.6 0.6 4 1.0m320 HAR11
Comet Magnitude Trend Observable When visible PanSTARRS (2015 ER61) 10.5 bright 45 N to 30 S early morning Johnson (2015 V2) 10.5 bright 90 N to 5 S morning 45P/Honda-Mrkos-Pajdusakova 11 bright 20 N to 30 S early evening NEOWISE (2016 U1) 11.5 bright 90 N to 5 N morning 144P/Kushida 12 fade 60 N to 35 S morning 237P/LINEAR 12 fade Poor elongation 43P/Wolf-Harrington 12.5 fade 45 N to 45 S early morning 2P/Encke 13 ? bright 65 N to 40 S evening 29P/Schwassmann-Wachmann 13 ? varies 10 N to 20 S early evening Spacewatch (2011 KP36) 13 fade 55 N to 50 S evening 81P/Wild 13.5 fade In conjunction PanSTARRS (2013 X1) 13.5 fade Poor elongation 41P/Tuttle-Giacobinni-Kresak [14 ? bright 50 N to 35 S morning
List of comets maintained by Jonathan Shanklin at http://www.ast.cam.ac.uk/~jds.
A new study has revealed similarities and relationships between certain types of chemicals found on 30 different comets, which vary widely in their overall composition compared to one another. The research is part of ongoing investigations into these primordial bodies, which contain material largely unchanged from the birth of the solar system some 4.6 billion years ago.
Based on computer simulations, Astrophysicists at the University of Bern, Switzerland, conclude that the comet Chury did not obtain its duck-like form during the formation of our solar system 4.5 billion years ago. Although it does contain primordial material, they are able to show that the comet in its present form is hardly more than a billion years old.
When the Rosetta spacecraft successfully touched down on comet 67P/Churyumov-Gerasimenko on September 30, 2016, the news was shared globally via Twitter in dozens of languages. Citizens the world over were engaged by the astronomical achievement, and now experts are eager to learn as much as possible about the critically important celestial body of ice.
We were saddened to learn the news yesterday that Klim Churyumov, who discovered Rosetta's comet together with Svetlana Gerasimenko in 1969, has passed away.
It’s been several years that a new method of processing CCD observations was announced by german astronomer Uwe Pilz. The method was a promising way for amateur astronomers, to generate a visual equivalent magnitude using a CCD measures with a very simple way of processing. Now after several years, there were several observers which were using this method, one of most active was Kevin Hills from United Kingdom. The huge amount of his observations made possible a deep comparative analysis of this method with visual and classic CCD magnitudes.