Observations of Comets C/2007 D1 (LINEAR), C/2007 D3 (LINEAR), C/2010 G3 (WISE), C/2010 S1 (LINEAR), and C/2012 K6 (McNaught) at large heliocentric distances

Ivanova, Oleksandra; Neslušan, L.; Krišandová, Zuzana Seman; Svoreň, J.; Корсун, П. П.; Afanasiev, V. L.; Reshetnyk, V.; Андреев, М. В.

doi:10.1016/j.icarus.2015.06.026

Cited by 17 publications

(7 citation statements)

References 57 publications

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“…We observed this comet on the outward orbit between 5.70 AU (2008-03-31) and 7.24 AU (2009-04-19). Ivanova et al (2015) observed this comet about two weeks prior our fist observation, they derived derived an Afrho about 180-200 cm, which is consistent to our data.…”

Section: C/2007 D3 (Linear)supporting

confidence: 91%

“…?s orbit at 5.2 AU (Meech & Svoren 2004). The main mechanisms that have been proposed to explain cometary activity of comets at large heliocentric distances are: the transition phase between amorphous and crystalline water ice (Prialnik 1992, Capria et al 2002, the annealing of amorphous water ice (Meech et al 2009), and the sublimation of more volatile admixtures like CO and/or CO2. In the past two decades, observational campaigns have been made to reveal the distant activity of comets, most by with observations of the Jupiter family (Meech 1991, O'Ceallaigh et al 1995Meech & Hainaut 1997;Lowry et al 1999;Szabó et al 2001;Szabó et al 2002;Korsun & Chörny 2003;Tozzi et al 2003;Szabó et al 2008;Mazzotta Epifani et al 2009;Meech et al 2009;Mazzotta Epifani et al 2010;Korsun et al 2010;Szabó et al 2012;Mazzotta Epifani et al 2014;Shi et al 2014;Ivanova et al 2015). However, there is still a lack in the observations of LP comets beyond 5.2 AU.…”

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confidence: 99%

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ACTIVITY OF 50 LONG-PERIOD COMETS BEYOND 5.2 au

Sárneczky

Szabó

Csák

et al. 2016

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Remote investigations of the ancient solar system matter has been traditionally carried out through the observations of long-period (LP) comets that are less affected by solar irradiation than the short-period counterparts orbiting much closer to the Sun. Here we summarize the results of our decade-long survey of the distant activity of LP comets. We found that the most important separation in the dataset is based on the dynamical nature of the objects. Dynamically new comets are characterized by a higher level of activity on average: the most active new comets in our sample can be characterized by Af ρ values >3-4 higher than that of our most active returning comets. New comets develop more symmetric comae, suggesting a generally isotropic outflow. Contrary to this, the coma of recurrent comets can be less symmetrical, ocassionally exhibiting negative slope parameters, suggesting sudden variations in matter production. The morphological appearance of the observed comets is rather diverse. A surprisingly large fraction of the comets have long, teniouos tails, but the presence of impressive tails does not show a clear correlation with the brightness of the comets.

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Section: C/2007 D3 (Linear)supporting

confidence: 91%

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confidence: 99%

ACTIVITY OF 50 LONG-PERIOD COMETS BEYOND 5.2 au

Sárneczky

Szabó

Csák

et al. 2016

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“…Also, it was considered that the nature of the dust particles presented in cometary coma does not depend on the heliocentric distance (Dollfus et al 1988). However, new investigations show differences between the activity of comets close to the Sun and distant comets (see, e.g., Mazzotta Epifani et al 2007Ivanova et al 2011Ivanova et al , 2015bDlugach et al 2018). Most likely the particles which form the comae are different.…”

Section: Discussionmentioning

confidence: 99%

Photometry, spectroscopy, and polarimetry of distant comet C/2014 A4 (SONEAR)

Ivanova

Lukyanyk

Kolokolova

et al. 2019

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Context. The study of distant comets, which are active at large heliocentric distances, is important for better understanding of their physical properties and mechanisms of long-lasting activity. Aims. We analyze the dust environment of the distant comet C/2014 A4 (SONEAR), with a perihelion distance near 4.1 au, using comprehensive observations obtained by different methods. Methods. We present an analysis of spectroscopy, photometry, and polarimetry of comet C/2014 A4 (SONEAR), which were performed on November 5 -7, 2015, when its heliocentric distance was 4.2 au and phase angle was 4.7 • . Long-slit spectra and photometric and linear polarimetric images were obtained using the focal reducer SCORPIO-2 attached to the prime focus of the 6-m telescope BTA (SAO RAS, Russia). We simulated the behavior of color and polarization in the coma presenting the cometary dust as a set of polydisperse polyshapes rough spheroids. Results. No emissions were detected in the 3800 -7200 Å wavelength range. The continuum showed a reddening effect with the normalized gradient of reflectivity 21.6±0.2% per 1000 Å within the 4650 -6200 Å wavelength region. The fan-like structure in the sunward hemisphere was detected. The radial profiles of surface brightness differ for r-sdss and g-sdss filters, indicating predominance of submicron and micron-sized particles in cometary coma. The dust color (g-r) varies from 0.75±0.05 m to 0.45±0.06 m along the tail. For aperture radius near 20 000 km, the dust productions in various filters were estimated as A f ρ = 680±18 cm (r-sdss) and 887±16 cm (g-sdss). The polarization map showed spatial variations of polarization over the coma from about -3% near the nucleus to -8% at cometocentric distance about 150 000 km. Our simulations show that the dust particles were dominated (or covered) by ice and tholin-like organics. Spatial changes in the color and polarization can be explained by particle fragmentation.

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“…We refer the Reader to Ivanova et al (2015Ivanova et al ( , 2016 Siding Spring (Australia). Basic parameters of the telescopes are given in Table 1.…”

Section: Techniques Of Observation and Data Processingmentioning

confidence: 99%

Colour variations of Comet C/2013 UQ4 (Catalina)

Ivanova

Zubko

Videen

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We report observations of color in the inner coma of Comet C/2013 UQ4 (Catalina) with the broadband B and R filters. We find significant temporal variations of the color slope, ranging from -12.67 ± 8.16% per 0.1 m up to 35.09 ± 11.70% per 0.1 m. It is significant that the comet changes color from red to blue over only a two-day period. Such dispersion cannot be characterized with an average color slope. We also observe Comet C/2013 UQ4 (Catalina) in infrared using Spitzer and find no significant CO/CO 2 gaseous species in its coma. Therefore, we classify Comet C/2013 UQ4 (Catalina) as a dust-rich comet and attribute the measured color slope to its dust. We analyze the color slope using the model of agglomerated debris particles and conclude that the C/2013 UQ4 coma was chemically heterogeneous, consisting of at least two components. The first component producing the bluest color is consistent with Mg-rich silicates.There are three different options for the second component producing the reddest color. This color is consistent with either Mg-Fe silicates, kerogen type II, or organic matter processed with a low dose of UV radiation.

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Observations of Comets C/2007 D1 (LINEAR), C/2007 D3 (LINEAR), C/2010 G3 (WISE), C/2010 S1 (LINEAR), and C/2012 K6 (McNaught) at large heliocentric distances

Cited by 17 publications

References 57 publications

ACTIVITY OF 50 LONG-PERIOD COMETS BEYOND 5.2 au

ACTIVITY OF 50 LONG-PERIOD COMETS BEYOND 5.2 au

Photometry, spectroscopy, and polarimetry of distant comet C/2014 A4 (SONEAR)

Colour variations of Comet C/2013 UQ4 (Catalina)

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