The Wayback Machine - https://web.archive.org/web/20160603180919/http://adsabs.harvard.edu/abs/2000P&SS...48..143P
Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· References in the article
· Citations to the Article (32) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Further investigations of random models of Uranus and Neptune
Authors:
Podolak, M.; Podolak, J. I.; Marley, M. S.
Affiliation:
AA(Department of Geophysics and Planetary Sciences, Tel Aviv University, Tel Aviv, Israel), AB(Department of Computer Science, Hebrew University, Jerusalem, Israel), AC(Department of Astronomy, New Mexico State University, Las Cruces, New Mexico, USA)
Publication:
Planetary and Space Science, Volume 48, Issue 2-3, p. 143-151. (P&SS; Homepage)
Publication Date:
02/2000
Origin:
ELSEVIER
Abstract Copyright:
(c) 2000 Elsevier Science Ltd
DOI:
10.1016/S0032-0633(99)00088-4
Bibliographic Code:
2000P&SS...48..143P

Abstract

We present a series of computer models for Uranus and Neptune where the interior density distribution is randomly chosen. The only constraints placed on the distribution are that the density does not decrease with decreasing radius, and that the density distribution fits the observed mass and gravitational moments of these planets. Previous models of these planets all had a density discontinuity at about 70% of the total radius. We use our models to explore the space of density distributions that fit the observed gravitational moments, and set limits on the position and size of this discontinuity. We find that models are possible with no discontinuity in the mantle. In addition a density discontinuity as large as 3 g cm -3 is possible for Uranus if the discontinuity is inward of about 0.75 Uranus radii. Closer to the surface the discontinuity must be smaller. For Neptune, the larger uncertainties in the measured moments result in coarser limits on the size of the density jump. Other means of limiting the range of acceptable models are discussed.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

  New!

Find Similar Abstracts:

Use: Authors
Title
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints
    



Morty Proxy This is a proxified and sanitized view of the page, visit original site.