The Pluto System After New Horizons最新文献

Transneptunian Space and the Post-Pluto Paradigm 跨海王星空间和后冥王星范式

The Pluto System After New Horizons Pub Date : 2021-07-05 DOI: 10.2458/azu_uapress_9780816540945-ch023

A. Parker

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引用次数: 1

Impact Craters on Pluto and Charon and Terrain Age Estimates 冥王星和冥卫一上的撞击坑和地形年龄估计

The Pluto System After New Horizons Pub Date : 2020-08-24 DOI: 10.2458/azu_uapress_9780816540945-ch007

K. Singer, S. Greenstreet, P. Schenk, S. Robbins, V. Bray

{"title":"Impact Craters on Pluto and Charon and Terrain Age Estimates","authors":"K. Singer, S. Greenstreet, P. Schenk, S. Robbins, V. Bray","doi":"10.2458/azu_uapress_9780816540945-ch007","DOIUrl":"https://doi.org/10.2458/azu_uapress_9780816540945-ch007","url":null,"abstract":"Pluto's terrains display a diversity of crater retention ages ranging from areas with no identifiable craters to heavily cratered terrains. This variation in crater densities is consistent with geologic activity occurring throughout Pluto's history and also a variety of resurfacing styles, including both exogenic and endogenic processes. Using estimates of impact flux and cratering rates over time, Pluto's heavily cratered terrains appear to be relatively ancient, 4 Ga or older. Charon's smooth plains, informally named Vulcan Planitia, did experience early resurfacing, but there is a relatively high spatial density of craters on Vulcan Planitia and almost all overprint the other types of volcanic or tectonic features. Both Vulcan Planitia and the northern terrains on Charon are also estimated to be ancient, 4 Ga or older. The craters on Pluto and Charon also show a distinct break in their size-frequency distributions (SFDs), where craters smaller than approximately 10-15 km in diameter have a shallower SFD power-law slope than those larger than this break diameter. This SFD shape on Pluto and Charon is different than what is observed on the Earth's Moon, and gives the Kuiper belt impactor SFD a different shape than that of the asteroid belt.","PeriodicalId":393977,"journal":{"name":"The Pluto System After New Horizons","volume":"158 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-08-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"133028570","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 5

Pluto’s Volatile and Climate Cycles on Short and Long Timescales 冥王星的挥发性和气候周期在短期和长期的时间尺度

The Pluto System After New Horizons Pub Date : 2019-07-01 DOI: 10.2458/azu_uapress_9780816540945-ch014

A. Earle, R. Binzel, L. Young, T. Bertrand, M. Buie, D. Cruikshank, K. Ennico, F. Forget, W. Grundy, J. Moore, C. Olkin, B. Schmitt, J. Spencer, J. Stansberry, S. Stern, L. Trafton, O. Umurhan, H. Weaver

{"title":"Pluto’s Volatile and Climate Cycles on Short and Long Timescales","authors":"A. Earle, R. Binzel, L. Young, T. Bertrand, M. Buie, D. Cruikshank, K. Ennico, F. Forget, W. Grundy, J. Moore, C. Olkin, B. Schmitt, J. Spencer, J. Stansberry, S. Stern, L. Trafton, O. Umurhan, H. Weaver","doi":"10.2458/azu_uapress_9780816540945-ch014","DOIUrl":"https://doi.org/10.2458/azu_uapress_9780816540945-ch014","url":null,"abstract":"The volatiles on Pluto’s surface, N2, CH4, and CO, are present in its atmosphere as well. The movement of volatiles affects Pluto’s surface and atmosphere on multiple timescales. On diurnal timescales, N2 is transported from areas of high to low insolation, and the latent heat of sublimation or condensation maintains a nearly isobaric atmosphere. On seasonal (orbital) timescales, Pluto’s atmosphere changes its 20 pressure by orders of magnitude, but most models predict that it is unlikely to collapse even at aphelion due to the equatorial N2 source in Sputnik Planitia and the high thermal inertia of the subsurface. On seasonal timescales, meters of N2 ice are transported across Pluto’s surface, but it is not yet clear from models how much of this transport is between areas which maintain N2 over an entire year (such as Sputnik Planitia) and to what extent deposition creates new volatile-covered areas (of either N2-rich or CH4-rich ice) or sublimation reveals underlying terrain. Pluto’s orbit and obliquity variations on ~3 Myr timescales (a Milankovitch cycle) induce considerable climate changes along with local accumulation or erosion of m-to-km thick layers of volatile ice. In a non-cyclical process, volatiles filled the large depression that is now Sputnik Planitia.","PeriodicalId":393977,"journal":{"name":"The Pluto System After New Horizons","volume":"32 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2019-07-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"127140627","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 7

Surface Composition of Pluto 冥王星的表面组成

The Pluto System After New Horizons Pub Date : 1900-01-01 DOI: 10.2458/azu_uapress_9780816540945-ch009

D. Cruikshank

引用次数: 0

Atmospheric Escape 大气逃逸

The Pluto System After New Horizons Pub Date : 1900-01-01 DOI: 10.2458/azu_uapress_9780816540945-ch015

D. Strobel

引用次数: 5

The Small Satellites of Pluto 冥王星的小卫星

The Pluto System After New Horizons Pub Date : 1900-01-01 DOI: 10.2458/azu_uapress_9780816540945-ch020

S. Porter

引用次数: 3

Charon: Colors and Photometric Properties 冥卫一:颜色和光度特性

The Pluto System After New Horizons Pub Date : 1900-01-01 DOI: 10.2458/azu_uapress_9780816540945-ch018

C. J. A. Howestt

引用次数: 2