Linking the collisional history of the main asteroid belt to its dynamical excitation and depletion

Bottke, W. F.; Durda, D. D.; Nesvorný, David; Jedicke, Robert; Morbidelli, Alessandro; Vokrouhlický, David; Levison, Harold F.

doi:10.1016/j.icarus.2005.05.017

Cited by 431 publications

(447 citation statements)

References 146 publications

Supporting

Mentioning

420

Contrasting

Unclassified

Order By: Relevance

“…A collision between a 100m and 10m asteroid might create a dust cloud that lasts sufficiently long to be identified as a 'transient moving object'. The collision rates in this size range Bottke et al(2005) imply that PS1 might identify one such event per month but this estimate is almost entirely dependent upon how long the dust clouds remains at an optical depth greater than one.…”

Section: Pan-starrs and The Solar Systemmentioning

confidence: 99%

The next decade of Solar System discovery with Pan-STARRS

et al. 2006

View full text Add to dashboard Cite

Abstract.The Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) at the University of Hawaii's Institute for Astronomy is a funded project to repeatedly survey the entire visible sky to faint limiting magnitudes (mR ∼ 24). It will be composed of four 1.8m diameter apertures each outfitted with fast readout orthogonal transfer Giga-pixel CCD cameras. A single aperture prototype telescopes is achieved first-light in the second half of 2006 with the full system becoming available a few years later. Roughly 60% of the surveying will be suitable for discovery of new solar system objects and it will cover the ecliptic, opposition and low solarelongation regions. In a single lunation Pan-STARRS will detect about five times more solar system objects than the entire currently known sample. Within its first year Pan-STARRS will have detected 20,000 Kuiper Belt Objects and by the end of its ten year operational lifetime we expect to have found 10 7 Main Belt objects and achieve ∼90% observational completeness for all NEOs larger than ∼300m diameter. With these data in hand Pan-STARRS will revolutionize our knowledge of the contents and dynamical structure of the solar system.Keywords. Keyword1, keyword2, keyword3, etc. Pan-STARRS OverviewThe conceptual design of the Pan-STARRS system derives from a desire to survey the sky as deeply, rapidly and inexpensively as possible. Relatively simple technological and economic arguments suggest that the minimum cost for a surveying system is achieved with telescope mirrors in the range of 1.5m to 2.5m diameter. Simply put, it is more cost effective to build more small telescopes to reach the same effective limiting magnitude and sky-coverage as a massive system due to the fact that duplicating a small system increases costs linearly while the cost of a single large system increases as a power of its light gathering ability. Another major benefit of a distributed aperture system is the reduced time to deployment over a monolithic system with equivalent etendue. Thus, Pan-STARRS opted to develop a design for a coordinated set of four small telescopes with the capability of a large synoptic survey system.A prototype single Pan-STARRS telescope (PS1) on Haleakala is nearing completion and is expected to start survey operations in mid to late 2007. It is designed to act as a test-bed for the commissioning, testing, and calibration of the Pan-STARRS hardware and software in anticipation of the full (four aperture) Pan-STARRS array. PS1 uses a 1.8m primary mirror to image a roughly 7 square degree field on a 1.4 Gigapixel CCD camera. With 0.26 arcsecond pixels, the images from PS1 will be well-matched to the sub-arcsecond seeing of Haleakala. The large entendue of PS1 will make it the most † for the Pan-STARRS team.

show abstract

Section: Pan-starrs and The Solar Systemmentioning

confidence: 99%

The next decade of Solar System discovery with Pan-STARRS

et al. 2006

View full text Add to dashboard Cite

show abstract

“…Smaller objects are collisionally destroyed on statistically shorter timescales relative to larger objects (Cheng 2004;Bottke et al 2005), meaning that currently existing smaller objects are statistically more likely to have been recently formed (e.g., in the fragmentation of a larger parent body) than larger bodies. The young families resulting from those fragmentation events may perhaps simply have not yet been identified because an insufficient number of members have been discovered to date, preventing the identification of the families by standard clustering analyses.…”

Section: Family Originsmentioning

confidence: 99%

The Main Belt Comets and ice in the Solar System

Snodgrass

Agarwal

Combi

et al. 2017

Astron Astrophys Rev

View full text Add to dashboard Cite

We review the evidence for buried ice in the asteroid belt; specifically the questions around the so-called Main Belt Comets (MBCs). We summarise the evidence for water throughout the Solar System, and describe the various methods for detecting it, including remote sensing from ultraviolet to radio wavelengths. We review progress in the first decade of study of MBCs, including observations, modelling of ice survival, and discussion on their origins. We then look at which methods will likely be most effective for further progress, including the key challenge of direct detection of (escaping) water in these bodies.

show abstract

“…However, crater distributions observed on asteroids show similarities to the crater distributions observed on the terrestrial planets, leading to the assumption that both types of body were impacted by the same projectile population and with a similar flux (Neukum and Ivanov, 1994;Ivanov et al, 2002;Schmedemann et al, 2014). Nevertheless, in recent years, our understanding of the main asteroid belt has greatly improved, both in terms of its past dynamical evolution and the current size-frequency distribution (e.g., Bottke et al, 2005;Morbidelli et al, 2010Morbidelli et al, , 2012. These improvements allowed the Dawn Science Team to build both a ''model'' crater chronology (that is not calibrated on radiometric ages) for main belt asteroids that is consistent with the current models of main belt evolution (O'Brien et al, 2014) and a crater chronology for main belt asteroids that is derived from the radiometrically calibrated lunar chronology .…”

Section: Absolute Agesmentioning

confidence: 99%

The chronostratigraphy of protoplanet Vesta

Williams

Jaumann

McSween

et al. 2014

Icarus

View full text Add to dashboard Cite

a b s t r a c tIn this paper we present a time-stratigraphic scheme and geologic time scale for the protoplanet Vesta, based on global geologic mapping and other analyses of NASA Dawn spacecraft data, complemented by insights gained from laboratory studies of howardite-eucrite-diogenite (HED) meteorites and geophysical modeling. On the basis of prominent impact structures and their associated deposits, we propose a time scale for Vesta that consists of four geologic time periods: Pre-Veneneian, Veneneian, Rheasilvian, and Marcian. The Pre-Veneneian Period covers the time from the formation of Vesta up to the Veneneia impact event, from 4.6 Ga to >2.1 Ga (using the asteroid flux-derived chronology system) or from 4.6 Ga to 3.7 Ga (under the lunar-derived chronology system). The Veneneian Period covers the time span between the Veneneia and Rheasilvia impact events, from >2.1 to 1 Ga (asteroid flux-derived chronology) or from 3.7 to 3.5 Ga (lunar-derived chronology), respectively. The Rheasilvian Period covers the time span between the Rheasilvia and Marcia impact events, and the Marcian Period covers the time between the Marcia impact event until the present. The age of the Marcia impact is still uncertain, but our current best estimates from crater counts of the ejecta blanket suggest an age between $120 and 390 Ma, depending upon choice of chronology system used. Regardless, the Marcia impact represents the youngest major geologic event on Vesta. Our proposed four-period geologic time scale for Vesta is, to a first order, comparable to those developed for other airless terrestrial bodies.

show abstract

Linking the collisional history of the main asteroid belt to its dynamical excitation and depletion

Cited by 431 publications

References 146 publications

The next decade of Solar System discovery with Pan-STARRS

The next decade of Solar System discovery with Pan-STARRS

The Main Belt Comets and ice in the Solar System

The chronostratigraphy of protoplanet Vesta

Contact Info

Product

Resources

About