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4 edition of Collisional time scales in the Kuiper disk and their implications found in the catalog.

Collisional time scales in the Kuiper disk and their implications

Collisional time scales in the Kuiper disk and their implications

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Published by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC, Springfield, Va .
Written in English


Edition Notes

StatementS. Alan Stern.
Series[NASA contractor report] -- NASA-CR-203206., NASA contractor report -- NASA CR-203206.
ContributionsUnited States. National Aeronautics and Space Administration.
The Physical Object
FormatMicroform
Pagination1 v.
ID Numbers
Open LibraryOL17593617M
OCLC/WorldCa40642307

  Summarizing, based on the work of Nesvorný & Morbidelli and considering the evolution of Neptune required to explain the structure of the Kuiper Belt (Nesvorný a, b), our results indicate that the preferred initial configuration of the giant planets at the time of the dissipation of the gas nebula is the , , , Cited by: Abstract The dust disks observed around mature stars are evidence that plantesimals are present in these systems on spatial scales that are similar to that of the asteroids and the Kuiper belt objects (KBOs) in the solar system.

CiteSeerX - Document Details (Isaac Councill, Lee Giles, Pradeep Teregowda): The dynamical evolution of Classical Kuiper Belt Objects (CKBOs) divides into two parts, according to the secular theory of test particle orbits. The first part is a forced oscillation driven by the planets, while the second part is a free oscillation whose amplitude is determined by the initial orbit of the test. Formation and Collisional Evolution of Kuiper Belt Objects Scott J. Kenyon Smithsonian Astrophysical Observatory the data are broadly consistent with KBO formation in a massive disk followed by substantial collisional grinding and dynamical ejection. However, there are important problems reconciling they lose their disks. For solar-type.

"Wide-Field CCD Survey For Bright Kuiper Belt Objects and Centaurs", Astron. J., , Stern, S. A. (). On the Number of Planets in the Outer Solar System: Evidence for a Substantial Population of km Bodies. Icarus, 90, Stern, S. A. (). Collisional Timescales in the Kuiper Disk and their Implications. Astron. These collisional lifetimes constrain the population of small (R > ~1 km) objects currently residing in the Kuiper Belt, and confirm that the size distribution slope at small size cannot be excessively steep - likely q ~ We track mutual semi-major axis, inclination, and eccentricity evolution through our simulations, and show that it is.


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Collisional time scales in the Kuiper disk and their implications Download PDF EPUB FB2

Collisional Time Scales in the Kuiper Disk and Their Implications - NASA/ADS We explore the rate of collisions among bodies in the present-day Kuiper Disk as a function the total mass and population size structure of the disk.

Get this from a library. Collisional time scales in the Kuiper disk and their implications. [Alan Stern; United States. National Aeronautics and Space Administration.]. We explore the rate of collisions among bodies in the present-day Kuiper Disk as a function of the total mass and population size structure of the disk.

We find that collisional evolution is an important evolutionary process in the disk as a whole, and indeed, that it is likely the dominant evolutionary process beyond approx. 42 AU, where dynamical instability time scales exceed the age of the solar : S.

Alan Stern. Collision time scales for impacts of 4-m-radius projectiles onto 1-km-radius comets range from 3×10 7, to 5×10 7 years. The cumulative fraction of the surface area of 1- and km-radius objects cratered by projectiles with radii larger than 4 m ranges from a few to a few tens percent over Gyr.

The flux of Edgeworth–Kuiper Belt projectiles onto Pluto and Charon is also calculated and is found to be ∼3–5 Cited by: Title: Collisional Time Scales in the Kuiper Disk and Their Implications Authors: Stern, S.

Journal: Astronomical Journal v, p Bibliographic Code: AJS. Complete bibliographic record Other article options Print this article; Previous article page Print this page. CiteSeerX - Document Details (Isaac Councill, Lee Giles, Pradeep Teregowda): We present results from our model of collision rates in the present-day Edgeworth-Kuiper Belt and Centaur region.

We have updated previous results to allow for new estimates of the total disk population, in order to examine surface activation and modification time scales due to cratering impacts. The Edgeworth—Kuiper (E—K) belt, a population of small bodies a thousand times greater in number than that of the main asteroid belt orbiting outside Neptune’s orbit, is undergoing collisional Cited by: 2.

In this case, if the collisional time scale is higher than this value then impacts might excavate material which is redder than the surface layer.

Such an effect could not be explored with the present simulations, since our model can only give accurate values of the relative collision rates, whereas absolute values are required in order to perform comparison with the competing reddening-darkening Cited by:   Asteroid shapes and hydration levels can serve as tracers of their history and origin.

For instance, the asteroids () Ryugu and () Bennu have an oblate spheroidal shape with a. During the period of rapid erosive mass loss, the disk probably exhibited optical depths of to - (reminiscent of β Pictoris), for a time scale of ˜ to ˜ years.

The Oort Cloud, the Kuiper belt and the Scattered Disk are dynamically distinct populations of small bodies evolving in the outer regions of the Solar System.

Whereas their collisional activity is now quiet, gravitational interactions with giant planets may have shaped these populations both dynamically and collisionally during their formation.

We explore the rate of collisions among bodies in the present-day Kuiper Disk as a function of the total mass and population size structure of the disk. We find that collisional evolution is an Author: Maria Antonietta Barucci. This paper presents the results of collisional evolution calculations for the Kuiper Belt starting from an initial size distribution similar to that produced by accretion simulations of that region—a steep power-law large object size distribution that breaks to a shallower slope at r ~ km, with collisional equilibrium achieved for objects r lsim by: FORMATION AND COLLISIONAL EVOLUTION OF KUIPER BELT OBJECTS Scott J.

Kenyon Smithsonian Astrophysical Observatory broadly consistent with KBO formation in a massive disk followed by substantial collisional grinding and dynamical ejection.

However, there are important problems reconciling the time. Thus, it is not clear whether grains can Cited by: Collisional time evolution of surface mass density in the Edgeworth-Kuiper Belt over 4 ×10 9 yr as a function of initial mass and mean-random orbital eccentricity.

In all nine cases shown, the initial disk mass is shown by a dotted line at %; in absolute terms, however, the initial disk mass declined with heliocentric distance as R   Stern, S.A. () On the collisional environment, accretion time scales and architecture of the massive primordial Kuiper belt, Astron.

– Tegler, S.C. and Romanishin, W. () The extraordinary colors of trans-Neptunian objects TB and SC, Icarus pp. – Author: R. Malhotra. Very little is known about the physical properties of Kuiper-belt objects1, due to their relatively small size and large distance from the Earth.

For example, a Kuiper Cited by: arXiv:astro-ph/v1 18 Jan Models of the Collisional DampingScenario for IceGiant Planets In this situation the disk is highly collisional, and the collisional damping is so efficient approximate time-scales are set equal to one another in order to determine zeroth-order.

We calculate the temperature of dust grains produced in Edgeworth-Kuiper Belt (EKB) based on the grain model for water-ice and silicate mixtures. The dust grains with radii ranging from μm to 1 mm have low temperatures of about 20 K to 50 K in EKB, depending on their size, solar distance, and a volume mixing ratio of silicate to by: 9.

Task 2: Collisional Modelling of the Kuiper Disk We have now completed the first model of collision rates of the Kuiper Disk. With this model we explored the rate of collisions among bodies in the present-day Kuiper Disk as a function of the total mass and population size structure of the Disk.

We find that collisional evolution is an. that can be applied to the physical effects of collisions in the Kuiper belt. We begin with observational evidence for significant past and present-day collisions in the Kuiper belt (section 2).

We then present a range of possible outcomes from collisions between KBOs (section 3) and discuss the principal discriminating factors (section 4.An annual report for STUDIES OF DISKS AROUND THE SUN AND OTHER STARS NASA Grant No.: NAGW of the total mass and population size structure of the Disk.

We find that collisional evolution is an important evolutionary process in the Disk as Collision Rates in the Kuiper Disk and Their Implications. S.A. Stern, The Astronomical Journal. Fig.

7 shows the catastrophic collisional lifetime of planetesimals of different sizes in the Fomalhaut disc for the three models of their collisional properties, using the size distribution inferred from the SED modelling (q d = ), assuming that this is truncated at and 10 km.

Normally a planetesimal is broken up by one that just Cited by: