Scientists investigate change in activity of comet 17P/Holmes
Time series of selected images of 17P/Holmes taken with an RC filter. All images have the standard orientation, that is, north is up and east to the left. At the bottom right in each image, solid vectors denote the orientation of the negative velocity of the comet, and dashed vectors show radial vectors outward from the solar direction. Credit: Yuna Grace Kwon et al., 2014.
(Phys.org)—Periodic comet 17P/Holmes is usually a very faint object. However, during its historic outburst in October 2007, when the comet’s coma expanded to a diameter greater than that of the sun, it became visible to the naked eye and was temporarily the largest object in our solar system. This event has drawn the attention of astronomers worldwide trying to investigate the comet’s uncertain and changing nature. 17P/Holmes has been intensively monitored during its perihelion passage in 2014 and the results of these observations were detailed in a paper published Dec. 29, 2014 on the arXiv pre-print server.
17P/Holmes is a Jupiter-family comet discovered by Edwin Holmes in 1892. Although the comet’s massive outburst event in 2007 was well-observed, very little is known about the long-term evolution in the activity of 17P/Holmes. The perihelion passage seven years later was expected to be a great occasion to study the comet in detail. Unfortunately, in March 2014, it passed its perihelion so far that there have been no published reports about the physical state of the comet during this passage.
Now, a research team led by Yuna Grace Kwon of the Seoul National University in South Korea, reports its photometric monitoring observations of the comet over a period of nearly two years from May 2013 to March 2015, including the 2014 perihelion passage. To monitor the comet’s activity, six ground-based telescopes were employed at five observatories: the Ishigakijima Astronomical Observatory (IAO), the Okayama Astrophysical Observatory (OAO), the Nishi-Harima Astronomical Observatory (NHAO), the Siding Spring Observatory (SSO), and the Bohyunsan Optical Astronomy Observatory (BOAO).
Thanks to these observations, the researchers were able to detect the comet’s circumnuclear dust coma and its feeble dust tail. They found out that the dust mass loss rate of 17P/Holmes’ inner dust coma has been declining with increasing heliocentric distance. They also noticed that the dust production rate became equivalent to the level before the 2007 outburst.
“The dust production rates around the 2014 perihelion passage were about five orders of magnitudes lower than the maximum value during the 2007 outburst, while they were comparable to that of the pre-outburst data,” the researchers wrote in the paper.
According to research team, this similarity suggests that the comet’s activity was restored to its former state, although it has shown lingering activity for years when it was around its aphelion.
They noted that the mass loss process yields valuable information for monitoring the activity of the 17P/Holmes.
Besides determining dust production rates, the scientists also calculated the diurnal skin depth and growth timescale of the comet’s dust mantle, inferring that it is now nearly five to seven centimeters thick and has been developing apace over the last seven years.