TRAPPIST photometry and imaging monitoring of comet C/2013 R1 (Lovejoy): Implications for the origin of daughter species

Opitom, Cyrielle; Jehin, Emmanuël; Manfroid, Jean; Hutsemékers, Damien; Gillon, M.; Magain, Pierre

doi:10.1051/0004-6361/201526427

Cited by 16 publications

(13 citation statements)

References 30 publications

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“…With our lower bound of Q(C 2 ) ≈ 5.1×10 23 s −1 , and the upper limit adopted from Kareta et al (2019), we find a bound on the slope γ < −10.6. This slope is significantly steeper than those of other comets in our Solar System, such as γ = −3.56 ± 0.16 for C/2013 R1 (Lovejoy) (Opitom et al 2015), γ = −4.10 ± 0.10 for 103P/Hartley 2 (Knight & Schleicher 2013), and γ = −2.60 to −4.39 for 81P/Wild 2 (Lin et al 2012). The steeper slope for 2I/Borisov suggests that its C 2 production rate might be more sensitive to the heliocentric distance r h than the Solar System comets.…”

Section: Discussionmentioning

confidence: 57%

Detection of Diatomic Carbon in 2I/Borisov

Lin

Lee

Gerdes

et al. 2020

ApJL

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2I/Borisov is the first-ever observed interstellar comet (and the second detected interstellar object). It was discovered on 30 August 2019 and has a heliocentric orbital eccentricity of ∼ 3.35, corresponding to a hyperbolic orbit that is unbound to the Sun. Given that it is an interstellar object, it is of interest to compare its properties -such as composition and activity -with the comets in our Solar System. This study reports low-resolution optical spectra of 2I/Borisov. The spectra were obtained by the MDM observatory Hiltner 2.4m telescope/Ohio State Multi-Object Spectrograph (on October 31.5 and November 4.5, 2019 UT). The wavelength coverage spanned from 3700Å to 9200Å. The dust continuum reflectance spectra of 2I/Borisov show that the spectral slope is steeper in the blue end of the spectrum (compared to the red). The spectra of 2I/Borisov clearly show CN emission at 3880Å, as well as C 2 emission at both 4750Å and 5150Å. Using a Haser model to covert the observed fluxes into estimates for the molecular production rates, we find Q(CN) = 2.4 ± 0.2 × 10 24 s −1 , and Q(C 2 ) = 5.5 ± 0.4 × 10 23 s −1 at the heliocentric distance of 2.145 au. Our Q(CN) estimate is consistent with contemporaneous observations, and the Q(C 2 ) estimate is generally below the upper limits of previous studies. We derived the ratio Q(C 2 )/Q(CN) = 0.2 ± 0.1, which indicates that 2I/Borisov is depleted in carbon chain species, but is not empty. This feature is not rare for the comets in our Solar System, especially in the class of Jupiter Family Comets.

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Section: Discussionmentioning

confidence: 57%

Detection of Diatomic Carbon in 2I/Borisov

Lin

Lee

Gerdes

et al. 2020

ApJL

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“…On the other hand, water production rates determined from water IR emissions with NIRSPEC at the Keck Observatory by Paganini et al (2014) over the pre-perihelion heliocentric distance range from 1.35 to 1.16 AU are systematically a factor of 2 or more below the SWAN values and the one overlapping value from . Similarly the ground-based nearultraviolet OH production rates given by Opitom et al (2015), after accounting for the ~0.82 OH yield from H 2 O photodissociation (Combi et al, 2004), like the NIRSPEC/Keck observations given by Paganini et al (2014), are systematically smaller by factors of 2 or more from the SWAN and IRAM rates. Figure 4b also shows various water production rate measures for comet C/2013 R1 (Lovejoy) determined from different observations.…”

Section: Results Of Model Analyses For Each Cometmentioning

confidence: 82%

“…Figure 4b also shows various water production rate measures for comet C/2013 R1 (Lovejoy) determined from different observations. Opitom et al (2015) have adopted the OH Haser scale lengths and methods from A' Hearn et al (1995) to calculate OH production rates. Schleicher and Osip (2002) has shown that in order to compare water production determined from OH observations with those of other methods that the production rates need to be corrected for the more appropriate vectorial model (Festou, 1981), which is more typically used by spacebased ultraviolet observations of OH (e.g., Swift by Bodewits et al, 2014).…”

Section: Results Of Model Analyses For Each Cometmentioning

confidence: 99%

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Water production activity of nine long-period comets from SOHO/SWAN observations of hydrogen Lyman-alpha: 2013–2016

Combi

Mäkinen

Bertaux

et al. 2018

Icarus

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Nine recently discovered long-period comets were observed by the Solar Wind Anisotropies Of these 9 comets 6 were long-period comets and 3 were possibly dynamically new. Water production rates were calculated from each of the 885 images using our standard time-resolved model that accounts for the whole water photodissociation chain, exothermic velocities and collisional escape of H atoms. For most of these comets there were enough observations over a broad enough range of heliocentric distances to calculate power-law fits to the variation of production rate with heliocentric distances for pre-and post-perihelion portions of the orbits.Comet C/2014 Q1 (PanSTARRS), with a perihelion distance of only ~0.3 AU, showed the most unusual variation of water production rate with heliocentric distance and the resulting active area variation, indicating that when the comet was within 0.7 AU its activity was dominated by the continuous release of icy grains and chunks, greatly increasing the active sublimation area by more than a factor of 10 beyond what it had at larger heliocentric distances. A possible interpretation suggests that a large fraction of the comet's mass was lost during the apparition.

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“…Used with the 2 × 2 binning mode it results in a pixel scale of 1.3 arcsec and a field of view of 22 arcmin. The observations of comet 67P have been performed once or twice a week in 2016 with a JohnsonCousins Rc filter and with exposure times ranging from 180 to 240 s. TRAPPIST images are reduced following a standard procedure described in Opitom et al (2015). The sky background is subtracted and the photometric calibration is performed using regular observations of photometric standard stars.…”

Section: Ground-based Observationsmentioning

confidence: 99%

The 2016 Feb 19 outburst of comet 67P/CG: an ESA Rosetta multi-instrument study

Grün

Agarwal

Altobelli

et al. 2016

Mon. Not. R. Astron. Soc.

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On 2016 Feb 19, nine Rosetta instruments serendipitously observed an outburst of gas and dust from the nucleus of comet 67P/Churyumov-Gerasimenko. Among these instruments were cameras and spectrometers ranging from UV over visible to microwave wavelengths, in situ gas, dust and plasma instruments, and one dust collector. At 09:40 a dust cloud developed at the edge of an image in the shadowed region of the nucleus. Over the next two hours the instruments recorded a signature of the outburst that significantly exceeded the background. The enhancement ranged from 50 per cent of the neutral gas density at Rosetta to factors >100 of the brightness of the coma near the nucleus. Dust related phenomena (dust counts or brightness due to illuminated dust) showed the strongest enhancements (factors >10). However, even the electron density at Rosetta increased by a factor 3 and consequently the spacecraft potential changed from ∼−16 V to −20 V during the outburst. A clear sequence

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TRAPPIST photometry and imaging monitoring of comet C/2013 R1 (Lovejoy): Implications for the origin of daughter species

Cited by 16 publications

References 30 publications

Detection of Diatomic Carbon in 2I/Borisov

Detection of Diatomic Carbon in 2I/Borisov

Water production activity of nine long-period comets from SOHO/SWAN observations of hydrogen Lyman-alpha: 2013–2016

The 2016 Feb 19 outburst of comet 67P/CG: an ESA Rosetta multi-instrument study

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