A P/Wirtanen evolution model

Capria, M. T.; Capaccioni, F.; Coradini, A.; Sanctis, M. C. De; Espinasse, S.; Federico, C.; Orosei, R.; Salomone, M.

doi:10.1016/0032-0633(96)00016-5

Cited by 41 publications

(30 citation statements)

References 30 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Water ice does not sublimate beyond 6 AU and CO and/or CO 2 must probably be invoked to explain such an activity at large heliocentric distances (Capria et al 1996). CO has indeed been marginally detected in June 1995 when Chiron was at 8.50 AU from the Sun by Womack & Stern (1997) who derived a production rate of 1.5 ± 0.8 × 10 28 s −1 .…”

Section: Visible Observationsmentioning

confidence: 99%

See 1 more Smart Citation

Properties of the nuclei of Centaurs Chiron and Chariklo

Groussin

Lamy

Jordá

2004

A&A

View full text Add to dashboard Cite

Abstract. We analyze visible, infrared, radio and spectroscopic observations of 2060 Chiron in a synthetic way to determine the physical properties of its nucleus. From visible observations performed from 1969 to 2001, we determine an absolute V magnitude for the nucleus of 7.28 ± 0.08 with an amplitude of 0.16 ± 0.03, implying a nearly spherical nucleus with a ratio of semi-axes a/b = 1.16 ± 0.03. Infrared observations at 25, 60, 100 and 160 µm (i.e., covering the broad maximum of the spectral energy distribution) obtained with the Infrared Space Observatory Photometer (ISOPHOT) in June 1996 when Chiron was near its perihelion are analyzed with a thermal model which considers an intimate mixture of water ice and refractory materials and includes heat conduction into the interior of the nucleus. We find a very low thermal inertia of 3and a radius of 71 ± 5 km. Combining the visible and infrared observations, we derive a geometric albedo of 0.11 ± 0.02. We find that the observed spectra of Chiron can be fitted by a mixture of water ice (∼30%) and refractory (∼70%) grains, and that this surface model has a geometric albedo consistent with the above value. We also analyze the visible, infrared and radio observations of Chariklo (1997 CU26) and derive a radius of 118 ± 6 km, a geometric albedo of 0.07 ± 0.01 and a thermal inertia of 0A mixture of water ice (∼20%) and refractory (∼80%) grains is compatible with the near-infrared spectrum and the above albedo.

show abstract

Section: Visible Observationsmentioning

confidence: 99%

“…During the 1987 to 1990 interval, when Chiron was beyond 11 AU from the Sun, a large brightening was observed which is not yet very well understood. At such a heliocentric distance, the activity is believed to be dominated by the sublimation of CO (Capria et al 1996).…”

Section: Introductionmentioning

confidence: 99%

Properties of the nuclei of Centaurs Chiron and Chariklo

Groussin

Lamy

Jordá

2004

A&A

View full text Add to dashboard Cite

show abstract

“…This might also introduce potentially large errors in the determination of the temperature distribution. We compared our results with a 1D model (Capria et al 1996) to evaluate the error made with the stratification assumption. For objects like TNOs, it has been found to be negligible (temperature differences less than 1%).…”

Section: Stratificationmentioning

confidence: 99%

New 3D thermal evolution model for icy bodies application to trans-Neptunian objects

Guilbert-Lepoutre

Lasue

Federico

et al. 2011

A&A

Self Cite

View full text Add to dashboard Cite

Context. Thermal evolution models have been developed over the years to investigate the evolution of thermal properties based on the transfer of heat fluxes or transport of gas through a porous matrix, among others. Applications of such models to trans-Neptunian objects (TNOs) and Centaurs has shown that these bodies could be strongly differentiated from the point of view of chemistry (i.e. loss of most volatile ices), as well as from physics (e.g. melting of water ice), resulting in stratified internal structures with differentiated cores and potential pristine material close to the surface. In this context, some observational results, such as the detection of crystalline water ice or volatiles, remain puzzling. Aims. In this paper, we would like to present a new fully three-dimensional thermal evolution model. With this model, we aim to improve determination of the temperature distribution inside icy bodies such as TNOs by accounting for lateral heat fluxes, which have been proven to be important for accurate simulations. We also would like to be able to account for heterogeneous boundary conditions at the surface through various albedo properties, for example, that might induce different local temperature distributions. Methods. In a departure from published modeling approaches, the heat diffusion problem and its boundary conditions are represented in terms of real spherical harmonics, increasing the numerical efficiency by roughly an order of magnitude. We then compare this new model and another 3D model recently published to illustrate the advantages and limits of the new model. We try to put some constraints on the presence of crystalline water ice at the surface of TNOs. Results. The results obtained with this new model are in excellent agreement with results obtained by different groups with various models. Small TNOs could remain primitive unless they are formed quickly (less than 2 Myr) or are debris from the disruption of larger bodies. We find that, for large objects with a thermal evolution dominated by the decay of long-lived isotopes (objects with a formation period greater than 2 to 3 Myr), the presence of crystalline water ice would require both a large radius (>300 km) and high density (>1500 kg m −3 ). In particular, objects with intermediate radii and densities would be an interesting transitory population deserving a detailed study of individual fates.

show abstract

“…The models of Capria et al (1996) and de Sanctis et al (1999) give a water production rate too low compared with the observations, althougth they assumed a 100% active surface. The models of Möhlmann (1999) and Benkhoff (1999) both made approximations when they calculate Q H 2 O : Möhlmann (1999) assumed an arbitrary active fraction of 50% of the illuminated hemisphere while Benkhoff (1999) calculated the water production rate at the sub-solar point, without taking into account the lower insolation at higher latitude and longitude.…”

Section: Introductionmentioning

confidence: 99%

Activity on the surface of the nucleus of comet 46P/Wirtanen

Groussin

Lamy

2003

A&A

View full text Add to dashboard Cite

Abstract. We present a thermal model of the nucleus of comet 46P/Wirtanen, constrained by the temporal variations of the water production rate, in order to understand the activity on its surface. We consider a spherical nucleus with a macroscopic mosaic of small and numerous active and inactive regions. At heliocentric distances r h > 1.5 AU, the active regions represent 5-15% of the surface. At ∼1.5 AU, a rapid increase takes place and the active fraction reaches 70 to 100% in about 10 days, and then remains approximately constant up to perihelion where Q H 2 O = 1.3 ± 0.3 × 10 28 molecule s −1 . Post-perihelion, this fraction returns to ∼10%. The model is consistent with a geometric albedo ≤0.06. A refractory crust likely forms post-perihelion and can explain the variations of the activity over an orbit. Finally, we derived an erosion of ∼0.5 m per revolution and a remaining lifetime for the nucleus of several hundred revolutions.

show abstract

A P/Wirtanen evolution model

Cited by 41 publications

References 30 publications

Properties of the nuclei of Centaurs Chiron and Chariklo

Properties of the nuclei of Centaurs Chiron and Chariklo

New 3D thermal evolution model for icy bodies application to trans-Neptunian objects

Activity on the surface of the nucleus of comet 46P/Wirtanen

Contact Info

Product

Resources

About