{"title":"直接成像太阳系外行星的日冕法","authors":"R. Terrile","doi":"10.1364/soa.1988.wa1","DOIUrl":null,"url":null,"abstract":"The goal of directly detecting the presence of planets around the nearby stars is one of great scientific interest and extreme difficulty. At visible wavelengths a Jupiter-sized planet around a nearby star 5 parsecs away is about one billion times fainter than the parent star and only 1 arcsec away. To extract such a small signal out of the background of scattered and diffracted light from the central star requires extraordinarily smooth optics at mid-spatial frequencies with instrumentation designed to reduce diffracted light.","PeriodicalId":184695,"journal":{"name":"Space Optics for Astrophysics and Earth and Planetary Remote Sensing","volume":"23 1","pages":"0"},"PeriodicalIF":0.0000,"publicationDate":"1900-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"Coronagraphic Methods for Direct Imaging of Extra-Solar Planets\",\"authors\":\"R. Terrile\",\"doi\":\"10.1364/soa.1988.wa1\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"The goal of directly detecting the presence of planets around the nearby stars is one of great scientific interest and extreme difficulty. At visible wavelengths a Jupiter-sized planet around a nearby star 5 parsecs away is about one billion times fainter than the parent star and only 1 arcsec away. To extract such a small signal out of the background of scattered and diffracted light from the central star requires extraordinarily smooth optics at mid-spatial frequencies with instrumentation designed to reduce diffracted light.\",\"PeriodicalId\":184695,\"journal\":{\"name\":\"Space Optics for Astrophysics and Earth and Planetary Remote Sensing\",\"volume\":\"23 1\",\"pages\":\"0\"},\"PeriodicalIF\":0.0000,\"publicationDate\":\"1900-01-01\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Space Optics for Astrophysics and Earth and Planetary Remote Sensing\",\"FirstCategoryId\":\"1085\",\"ListUrlMain\":\"https://doi.org/10.1364/soa.1988.wa1\",\"RegionNum\":0,\"RegionCategory\":null,\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"\",\"JCRName\":\"\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"Space Optics for Astrophysics and Earth and Planetary Remote Sensing","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.1364/soa.1988.wa1","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
Coronagraphic Methods for Direct Imaging of Extra-Solar Planets
The goal of directly detecting the presence of planets around the nearby stars is one of great scientific interest and extreme difficulty. At visible wavelengths a Jupiter-sized planet around a nearby star 5 parsecs away is about one billion times fainter than the parent star and only 1 arcsec away. To extract such a small signal out of the background of scattered and diffracted light from the central star requires extraordinarily smooth optics at mid-spatial frequencies with instrumentation designed to reduce diffracted light.
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