Comet P/2010 TO20 LINEAR-Grauer as a Mini-29P/SW1

Lacerda, Pedro

doi:10.1093/mnras/sts164

Cited by 12 publications

(23 citation statements)

References 37 publications

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“…This deviation, which should be considered as an upper limit, is completely negligible in the scale of variations we are dealing with in the dynamical analysis of the orbital evolution. This result is close to the one derived for Lacerda (2013), where the author gives the maximum semi-major deviation for P/2010 T020 LINEAR-Grauer as 0.42 AU. As a result of our 15 Myr backward integration for all targets, we find that the ∼98% of the particles are ejected before the end of the integration, and in almost all cases, the surviving clones are in the transneptunian region.…”

Section: Dynamical History Analysissupporting

confidence: 89%

“…In a later study of the same authors (Levison & Duncan 1997), they estimated that the physical lifetime of JFCs is between (3-25) × 10 3 yr, where the most likely value is 12 × 10 3 yr. In our case, we use the Mercury package version 6.2, a numerical integrator developed by Chambers (1999), to determine the dynamical evolution of our targets, that has been used by other authors with the same purpose (e.g., Hsieh et al 2012a,b;Lacerda 2013). Due to the chaotic nature of the targets, which was mentioned in the Levison & Duncan (1994) study, we generate a total of 99 clones having 2σ dispersion in three of the orbital elements: semi-major axis, eccentricity, and inclination (hereafter a, e, and i), where σ is the uncertainty in the corresponding parameter as given in the JPL Horizons online solar system data 1 .…”

Section: Discussionmentioning

confidence: 99%

“…In this study, we neglect the non-gravitational forces using the same arguments as Lacerda (2013). Thus, assuming that the non-gravitational acceleration, T , is due to a single sublimation jet tangential to the comet orbit, the change rate of the semi-major axis is described by…”

Section: Dynamical History Analysismentioning

confidence: 99%

“…The second part in our study is the analysis of the recent (15 Myr) dynamical history for each target. To perform this task, we use the numerical integrator developed by Chambers (1999) as did by other authors before (e.g., Hsieh et al 2012a,b;Lacerda 2013). This will serve to derive the time spent by each comet in each region and, specifically, in the Jupiter family region, where it is supposed that the comets become active periodically.…”

Section: Introductionmentioning

confidence: 99%

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Dust environment and dynamical history of a sample of short-period comets

Pozuelos¹,

Moreno²,

Aceituno³

et al. 2014

A&A

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Aims. In this work, we present an extended study of the dust environment of a sample of short-period comets and their dynamical history. With this aim, we characterize the dust tails when the comets are active, and we make a statistical study to determine their dynamical evolution. The targets selected were 22P/Kopff, 30P/Reinmuth 1, 78P/Gehrels 2, 115P/Maury, 118P/Shoemaker-Levy 4, 123P/West-Hartley, 157P/Tritton, 185/Petriew, and P/2011 W2 (Rinner). Methods. We use two different observational data sets: a set of images taken at the Observatorio de Sierra Nevada and, the A f ρ curves provided by the amateur astronomical association Cometas-Obs. To model these observations, we use our Monte Carlo dust tail code. From this analysis, we derive the dust parameters, which best describe the dust environment: dust loss rates, ejection velocities, and size distribution of particles. On the other hand, we use a numerical integrator to study the dynamical history of the comets, which allows us to determine with a 90% confidence level the time spent by these objects in the region of Jupiter family comets. Results. From the Monte Carlo dust tail code, we derived three categories according to the amount of dust emitted: weakly active (115P, 157P, and Rinner), moderately active (30P, 123P, and 185P), and highly active (22P, 78P, and 118P). The dynamical studies showed that the comets of this sample are young in the Jupiter family region, where the youngest ones are 22P (∼100 yr), 78P (∼500 yr), and 118P (∼600 yr). The study points to a certain correlation between comet activity and time spent in the Jupiter family region, although this trend is not always fulfilled. The largest particle sizes are not tightly constrained, so that the total dust mass derived should be regarded as a lower limit.

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Section: Dynamical History Analysissupporting

confidence: 89%

Section: Discussionmentioning

confidence: 99%

Section: Dynamical History Analysismentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Dust environment and dynamical history of a sample of short-period comets

Pozuelos¹,

Moreno²,

Aceituno³

et al. 2014

A&A

View full text Add to dashboard Cite

show abstract

“…In the second part of our study we analyze the dynamical history of these comets. To perform this task we use the numerical integrator developed by Chambers (1999), which has been used before by other authors, such as Hsieh et al (2012a,b) and Lacerda (2013). From this analysis we studied the last 15 Myr of these comets, and we obtained the time spent by them in the region of the Jupiter family Comets (JFCs).…”

Section: Introductionmentioning

confidence: 99%

Dust environment and dynamical history of a sample of short-period comets

Pozuelos

Moreno

Aceituno

et al. 2014

A&A

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Aims. This paper is a continuation of the first paper in this series, where we presented an extended study of the dust environment of a sample of short-period comets and their dynamical history. On this occasion, we focus on comets 81P/Wild 2 and 103P/Hartley 2, which are of special interest as targets of the spacecraft missions Stardust and EPOXI. Methods. As in the previous study, we used two sets of observational data: a set of images, acquired at Sierra Nevada and Lulin observatories, and the A f ρ data as a function of the heliocentric distance provided by the amateur astronomical association Cometas-Obs. The dust environment of comets (dust loss rate, ejection velocities, and size distribution of the particles) was derived from our Monte Carlo dust tail code. To determine their dynamical history we used the numerical integrator Mercury 6.2 to ascertain the time spent by these objects in the Jupiter family Comet region. Results. From the dust analysis, we conclude that both 81P/Wild 2 and 103P/Hartley 2 are dusty comets, with an annual dust production rate of 2.8 × 10 9 kg yr −1 and (0.4−1.5) × 10 9 kg yr −1 , respectively. From the dynamical analysis, we determined their time spent in the Jupiter family Comet region as ∼40 yr in the case of 81P/Wild 2 and ∼1000 yr for comet 103P/Hartley 2. These results imply that 81P/Wild 2 is the youngest and the most active comet of the eleven short-period comets studied so far, which tends to favor the correlation between the time spent in JFCs region and the comet activity previously discussed.

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