双近地小行星 2018 EB 的雷达和光学观测及物理建模

IF 3.8 Q2 ASTRONOMY & ASTROPHYSICS The Planetary Science Journal Pub Date : 2024-05-27 DOI:10.3847/psj/ad4342
Marina Brozović, Lance A. M. Benner, Shantanu P. Naidu, Nicholas Moskovitz, Jon D. Giorgini, Anne K. Virkki, Sean E. Marshall, Lord R. Dover, Agata Rożek, Stephen C. Lowry, Brian D. Warner, Patrick A. Taylor, Edgard G. Rivera-Valentin, Timothy A. Lister, Joseph P. Chatelain, Michael W. Busch, Christopher Magri, Joseph S. Jao, Lawrence G. Snedeker and Kenneth J. Lawrence
{"title":"双近地小行星 2018 EB 的雷达和光学观测及物理建模","authors":"Marina Brozović, Lance A. M. Benner, Shantanu P. Naidu, Nicholas Moskovitz, Jon D. Giorgini, Anne K. Virkki, Sean E. Marshall, Lord R. Dover, Agata Rożek, Stephen C. Lowry, Brian D. Warner, Patrick A. Taylor, Edgard G. Rivera-Valentin, Timothy A. Lister, Joseph P. Chatelain, Michael W. Busch, Christopher Magri, Joseph S. Jao, Lawrence G. Snedeker and Kenneth J. Lawrence","doi":"10.3847/psj/ad4342","DOIUrl":null,"url":null,"abstract":"We report radar, photometric, and visible-wavelength spectrophotometry observations of NEA 2018 EB obtained in 2018. The radar campaign started at Goldstone (8560 MHz, 3.5 cm) on April 7, and it was followed by more extensive observations from October 5 to 9 by both Arecibo (2380 MHz, 12.6 cm) and Goldstone. 2018 EB was observed optically on April 5, 8, and 9 and again on October 18. Spectrophotometry was obtained on October 19 with the SOAR telescope, and the data suggest that 2018 EB is an Xk-class object. The echo power spectra and delay-Doppler radar images revealed that 2018 EB is a binary system. Radar images constrained the satellite's diameter to km, but the data were not sufficient for shape modeling. Shape modeling of lightcurves and radar data yielded an oblate primary with an effective diameter D = 0.30 ± 0.04 km and a sidereal rotation period of hr. Measurements of delay-Doppler separations between the centers of mass of the primary and the satellite, along with the timing of a radar eclipse observed on October 9, resulted in an orbit fit for the satellite with a semimajor axis of km, an eccentricity of 0.15 ± 0.04, a period of hr, and an orbit pole constrained to the ecliptic longitudes and latitudes of and . The system mass was estimated to be kg, which yielded a bulk density of g cm−3. Our analysis suggests that 2018 EB has a low optical albedo of pV = 0.028 ± 0.016 and a relatively high radar albedo of ηOC = 0.29 ± 0.11 at Arecibo and η = 0.22 ± 0.10 at Goldstone.","PeriodicalId":34524,"journal":{"name":"The Planetary Science Journal","volume":"46 1","pages":""},"PeriodicalIF":3.8000,"publicationDate":"2024-05-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"Radar and Optical Observations and Physical Modeling of Binary Near-Earth Asteroid 2018 EB\",\"authors\":\"Marina Brozović, Lance A. M. Benner, Shantanu P. Naidu, Nicholas Moskovitz, Jon D. Giorgini, Anne K. Virkki, Sean E. Marshall, Lord R. Dover, Agata Rożek, Stephen C. Lowry, Brian D. Warner, Patrick A. Taylor, Edgard G. Rivera-Valentin, Timothy A. Lister, Joseph P. Chatelain, Michael W. Busch, Christopher Magri, Joseph S. Jao, Lawrence G. Snedeker and Kenneth J. Lawrence\",\"doi\":\"10.3847/psj/ad4342\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"We report radar, photometric, and visible-wavelength spectrophotometry observations of NEA 2018 EB obtained in 2018. The radar campaign started at Goldstone (8560 MHz, 3.5 cm) on April 7, and it was followed by more extensive observations from October 5 to 9 by both Arecibo (2380 MHz, 12.6 cm) and Goldstone. 2018 EB was observed optically on April 5, 8, and 9 and again on October 18. Spectrophotometry was obtained on October 19 with the SOAR telescope, and the data suggest that 2018 EB is an Xk-class object. The echo power spectra and delay-Doppler radar images revealed that 2018 EB is a binary system. Radar images constrained the satellite's diameter to km, but the data were not sufficient for shape modeling. Shape modeling of lightcurves and radar data yielded an oblate primary with an effective diameter D = 0.30 ± 0.04 km and a sidereal rotation period of hr. Measurements of delay-Doppler separations between the centers of mass of the primary and the satellite, along with the timing of a radar eclipse observed on October 9, resulted in an orbit fit for the satellite with a semimajor axis of km, an eccentricity of 0.15 ± 0.04, a period of hr, and an orbit pole constrained to the ecliptic longitudes and latitudes of and . The system mass was estimated to be kg, which yielded a bulk density of g cm−3. Our analysis suggests that 2018 EB has a low optical albedo of pV = 0.028 ± 0.016 and a relatively high radar albedo of ηOC = 0.29 ± 0.11 at Arecibo and η = 0.22 ± 0.10 at Goldstone.\",\"PeriodicalId\":34524,\"journal\":{\"name\":\"The Planetary Science Journal\",\"volume\":\"46 1\",\"pages\":\"\"},\"PeriodicalIF\":3.8000,\"publicationDate\":\"2024-05-27\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"The Planetary Science Journal\",\"FirstCategoryId\":\"1085\",\"ListUrlMain\":\"https://doi.org/10.3847/psj/ad4342\",\"RegionNum\":0,\"RegionCategory\":null,\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"Q2\",\"JCRName\":\"ASTRONOMY & ASTROPHYSICS\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"The Planetary Science Journal","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.3847/psj/ad4342","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q2","JCRName":"ASTRONOMY & ASTROPHYSICS","Score":null,"Total":0}
引用次数: 0

摘要

我们报告了2018年对NEA 2018 EB进行的雷达、测光和可见光波长分光光度观测。雷达观测活动于 4 月 7 日在金石(8560 MHz,3.5 厘米)开始,随后于 10 月 5 日至 9 日在阿雷西博(2380 MHz,12.6 厘米)和金石进行了更广泛的观测。4 月 5 日、8 日和 9 日对 2018 EB 进行了光学观测,10 月 18 日再次进行了观测。10 月 19 日用 SOAR 望远镜进行了分光光度测量,数据表明 2018 EB 是一个 Xk 级天体。回波功率谱和延迟多普勒雷达图像显示 2018 EB 是一个双星系。雷达图像将该卫星的直径限制在千米,但这些数据不足以进行形状建模。对光曲线和雷达数据进行形状建模后发现,2018 EB 的主星呈扁球形,有效直径 D = 0.30 ± 0.04 千米,恒星旋转周期为小时。通过测量主星和卫星质心之间的延迟-多普勒距离,以及 10 月 9 日观测到的雷达日食时间,拟合出卫星的轨道,半主轴为 km,偏心率为 0.15 ± 0.04,周期为 hr,轨道极点受限于黄道经度和纬度。系统质量估计为千克,体积密度为克厘米-3。我们的分析表明,2018 EB 的光学反照率较低,为 pV = 0.028 ± 0.016,雷达反照率相对较高,在阿雷西博为 ηOC = 0.29 ± 0.11,在金石为 η = 0.22 ± 0.10。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
查看原文
分享 分享
微信好友 朋友圈 QQ好友 复制链接
本刊更多论文
Radar and Optical Observations and Physical Modeling of Binary Near-Earth Asteroid 2018 EB
We report radar, photometric, and visible-wavelength spectrophotometry observations of NEA 2018 EB obtained in 2018. The radar campaign started at Goldstone (8560 MHz, 3.5 cm) on April 7, and it was followed by more extensive observations from October 5 to 9 by both Arecibo (2380 MHz, 12.6 cm) and Goldstone. 2018 EB was observed optically on April 5, 8, and 9 and again on October 18. Spectrophotometry was obtained on October 19 with the SOAR telescope, and the data suggest that 2018 EB is an Xk-class object. The echo power spectra and delay-Doppler radar images revealed that 2018 EB is a binary system. Radar images constrained the satellite's diameter to km, but the data were not sufficient for shape modeling. Shape modeling of lightcurves and radar data yielded an oblate primary with an effective diameter D = 0.30 ± 0.04 km and a sidereal rotation period of hr. Measurements of delay-Doppler separations between the centers of mass of the primary and the satellite, along with the timing of a radar eclipse observed on October 9, resulted in an orbit fit for the satellite with a semimajor axis of km, an eccentricity of 0.15 ± 0.04, a period of hr, and an orbit pole constrained to the ecliptic longitudes and latitudes of and . The system mass was estimated to be kg, which yielded a bulk density of g cm−3. Our analysis suggests that 2018 EB has a low optical albedo of pV = 0.028 ± 0.016 and a relatively high radar albedo of ηOC = 0.29 ± 0.11 at Arecibo and η = 0.22 ± 0.10 at Goldstone.
求助全文
通过发布文献求助,成功后即可免费获取论文全文。 去求助
来源期刊
The Planetary Science Journal
The Planetary Science Journal Earth and Planetary Sciences-Geophysics
CiteScore
5.20
自引率
0.00%
发文量
249
审稿时长
15 weeks
期刊最新文献
Jovian Vortex Hunter: A Citizen Science Project to Study Jupiter’s Vortices Experimental Method for Measuring Cohesion of Regolith via Electrostatic Lofting Mid-infrared Measurements of Ion-irradiated Carbonaceous Meteorites: How to Better Detect Space Weathering Effects Triton’s Captured Youth: Tidal Heating Kept Triton Warm and Active for Billions of Years The Global Distribution of Water and Hydroxyl on the Moon as Seen by the Moon Mineralogy Mapper (M3)
×
引用
GB/T 7714-2015
复制
MLA
复制
APA
复制
导出至
BibTeX EndNote RefMan NoteFirst NoteExpress
×
×
提示
您的信息不完整,为了账户安全,请先补充。
现在去补充
×
提示
您因"违规操作"
具体请查看互助需知
我知道了
×
提示
现在去查看 取消
×
提示
确定
0
微信
客服QQ
Book学术公众号 扫码关注我们
反馈
×
意见反馈
请填写您的意见或建议
请填写您的手机或邮箱
已复制链接
已复制链接
快去分享给好友吧!
我知道了
×
扫码分享
扫码分享
Book学术官方微信
Book学术文献互助
Book学术文献互助群
群 号:481959085
Book学术
文献互助 智能选刊 最新文献 互助须知 联系我们:info@booksci.cn
Book学术提供免费学术资源搜索服务,方便国内外学者检索中英文文献。致力于提供最便捷和优质的服务体验。
Copyright © 2023 Book学术 All rights reserved.
ghs 京公网安备 11010802042870号 京ICP备2023020795号-1