{"title":"抛物面屏幕照射下的黑洞图像","authors":"E. V. Mikheeva, S. V. Repin, V. N. Lukash","doi":"10.1134/S1063772924700057","DOIUrl":null,"url":null,"abstract":"<p>An analytical model of a parabolic screen illuminating a black hole is proposed. This allows to avoid naturally the appearance of edge effects associated with photons moving along the plane of the screen illuminating the black hole. The temperature distribution along the radius of the screen corresponds to that for a relativistic disk (Novikov–Thorne disk). It is shown that the structure of the emerging black hole shadow differs significantly from the case when the photon source is a remote screen, since in the model considered, the photons subjected to strong gravitational lensing of the black hole are emitted by the “back side” of the screen, which would not be visible in the absence of a black hole. In the thin screen approximation, the shadow of a Schwarzschild black hole has been constructed in cases when the angle between the axis of symmetry of the illuminating screen and the direction towards the observer is 5°, 30°, 60°, and 80°. The images for the Kerr black hole are shown for the angles of 60° and 80°.</p>","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 1","pages":"1 - 10"},"PeriodicalIF":1.1000,"publicationDate":"2024-05-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"Image of a Black Hole Illuminated by a Parabolic Screen\",\"authors\":\"E. V. Mikheeva, S. V. Repin, V. N. Lukash\",\"doi\":\"10.1134/S1063772924700057\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"<p>An analytical model of a parabolic screen illuminating a black hole is proposed. This allows to avoid naturally the appearance of edge effects associated with photons moving along the plane of the screen illuminating the black hole. The temperature distribution along the radius of the screen corresponds to that for a relativistic disk (Novikov–Thorne disk). It is shown that the structure of the emerging black hole shadow differs significantly from the case when the photon source is a remote screen, since in the model considered, the photons subjected to strong gravitational lensing of the black hole are emitted by the “back side” of the screen, which would not be visible in the absence of a black hole. In the thin screen approximation, the shadow of a Schwarzschild black hole has been constructed in cases when the angle between the axis of symmetry of the illuminating screen and the direction towards the observer is 5°, 30°, 60°, and 80°. The images for the Kerr black hole are shown for the angles of 60° and 80°.</p>\",\"PeriodicalId\":55440,\"journal\":{\"name\":\"Astronomy Reports\",\"volume\":\"68 1\",\"pages\":\"1 - 10\"},\"PeriodicalIF\":1.1000,\"publicationDate\":\"2024-05-08\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Astronomy Reports\",\"FirstCategoryId\":\"101\",\"ListUrlMain\":\"https://link.springer.com/article/10.1134/S1063772924700057\",\"RegionNum\":4,\"RegionCategory\":\"物理与天体物理\",\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"Q3\",\"JCRName\":\"ASTRONOMY & ASTROPHYSICS\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"Astronomy Reports","FirstCategoryId":"101","ListUrlMain":"https://link.springer.com/article/10.1134/S1063772924700057","RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q3","JCRName":"ASTRONOMY & ASTROPHYSICS","Score":null,"Total":0}
Image of a Black Hole Illuminated by a Parabolic Screen
An analytical model of a parabolic screen illuminating a black hole is proposed. This allows to avoid naturally the appearance of edge effects associated with photons moving along the plane of the screen illuminating the black hole. The temperature distribution along the radius of the screen corresponds to that for a relativistic disk (Novikov–Thorne disk). It is shown that the structure of the emerging black hole shadow differs significantly from the case when the photon source is a remote screen, since in the model considered, the photons subjected to strong gravitational lensing of the black hole are emitted by the “back side” of the screen, which would not be visible in the absence of a black hole. In the thin screen approximation, the shadow of a Schwarzschild black hole has been constructed in cases when the angle between the axis of symmetry of the illuminating screen and the direction towards the observer is 5°, 30°, 60°, and 80°. The images for the Kerr black hole are shown for the angles of 60° and 80°.
期刊介绍:
Astronomy Reports is an international peer reviewed journal that publishes original papers on astronomical topics, including theoretical and observational astrophysics, physics of the Sun, planetary astrophysics, radio astronomy, stellar astronomy, celestial mechanics, and astronomy methods and instrumentation.