{"title":"中质量恒星的隐藏伴星。XX.发现 p Puppis 的 0.58M ⊙, 7.4 au 伴星","authors":"I. Waisberg, Y. Klein, B. Katz","doi":"10.3847/2515-5172/ad5724","DOIUrl":null,"url":null,"abstract":"p Puppis is a nearby 3.1M ⊙ B8V star with astrometric evidence for a close companion in addition to its two wide companions at 1.3 kau (a white dwarf (WD)) and 38.7 kau (an F2V astrometric binary). Here we report on a VLTI/GRAVITY observation that revealed the close companion to be a 0.58M ⊙ star at a projected separation ρ = 100.2 mas ↔ 7.4 au, confirming the system to be a quintuple. The discovered companion explains the X-ray emission of p Pup detected by eROSITA. Moreover, we also find that the isochrone age of 100−20+50 Myr of p Pup is incompatible with the minimum cooling age of 350 Myr for the 1.3 kau wide WD companion, suggesting that either they are not coeval or that the WD was formed through a non-trivial channel.","PeriodicalId":74684,"journal":{"name":"Research notes of the AAS","volume":"52 49","pages":""},"PeriodicalIF":0.0000,"publicationDate":"2024-06-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"Hidden Companions to Intermediate-mass Stars. XX. Discovery of a 0.58M ⊙, 7.4 au Companion to p Puppis\",\"authors\":\"I. Waisberg, Y. Klein, B. Katz\",\"doi\":\"10.3847/2515-5172/ad5724\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"p Puppis is a nearby 3.1M ⊙ B8V star with astrometric evidence for a close companion in addition to its two wide companions at 1.3 kau (a white dwarf (WD)) and 38.7 kau (an F2V astrometric binary). Here we report on a VLTI/GRAVITY observation that revealed the close companion to be a 0.58M ⊙ star at a projected separation ρ = 100.2 mas ↔ 7.4 au, confirming the system to be a quintuple. The discovered companion explains the X-ray emission of p Pup detected by eROSITA. Moreover, we also find that the isochrone age of 100−20+50 Myr of p Pup is incompatible with the minimum cooling age of 350 Myr for the 1.3 kau wide WD companion, suggesting that either they are not coeval or that the WD was formed through a non-trivial channel.\",\"PeriodicalId\":74684,\"journal\":{\"name\":\"Research notes of the AAS\",\"volume\":\"52 49\",\"pages\":\"\"},\"PeriodicalIF\":0.0000,\"publicationDate\":\"2024-06-14\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Research notes of the AAS\",\"FirstCategoryId\":\"1085\",\"ListUrlMain\":\"https://doi.org/10.3847/2515-5172/ad5724\",\"RegionNum\":0,\"RegionCategory\":null,\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"\",\"JCRName\":\"\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"Research notes of the AAS","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.3847/2515-5172/ad5724","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
引用次数: 0
摘要
p Puppis 是一颗邻近的 3.1M ⊙ B8V 恒星，除了它在 1.3 kau（一颗白矮星（WD））和 38.7 kau（一颗 F2V 天体测量双星）的两个宽伴星之外，还有一个近伴星的天体测量证据。我们在这里报告的VLTI/GRAVITY观测结果显示，这个近伴星是一颗0.58M ⊙恒星，投影距离ρ = 100.2 mas ↔ 7.4 au，从而证实了这个系统是一个五倍体。发现的伴星解释了 eROSITA 探测到的 p Pup 的 X 射线发射。此外，我们还发现p Pup的等时年龄（100-20+50 Myr）与1.3 kau宽WD伴星的最小冷却年龄（350 Myr）不一致，这表明它们不是共生的，或者WD是通过一个非三维通道形成的。
Hidden Companions to Intermediate-mass Stars. XX. Discovery of a 0.58M ⊙, 7.4 au Companion to p Puppis
p Puppis is a nearby 3.1M ⊙ B8V star with astrometric evidence for a close companion in addition to its two wide companions at 1.3 kau (a white dwarf (WD)) and 38.7 kau (an F2V astrometric binary). Here we report on a VLTI/GRAVITY observation that revealed the close companion to be a 0.58M ⊙ star at a projected separation ρ = 100.2 mas ↔ 7.4 au, confirming the system to be a quintuple. The discovered companion explains the X-ray emission of p Pup detected by eROSITA. Moreover, we also find that the isochrone age of 100−20+50 Myr of p Pup is incompatible with the minimum cooling age of 350 Myr for the 1.3 kau wide WD companion, suggesting that either they are not coeval or that the WD was formed through a non-trivial channel.
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