{"title":"长周期变量中的 OH 和 H2O Maser 活动","authors":"Tian Wu and Graeme H. Smith","doi":"10.3847/2515-5172/ad660d","DOIUrl":null,"url":null,"abstract":"The distribution within an infrared color–magnitude diagram of variable red giants known to have circumstellar masers is reported. Stars with H2O-maser sources occur within a color and period domain of (J − Ks) > 1.15 and P > 199 days, respectively, often in the absence of OH masers. By contrast, OH masers are mostly detected among cooler red giants with (J − Ks) > 1.35 and P > 316 days, and can coexist with H2O-maser sources. The results suggest that red giants must evolve to absolute magnitudes brighter than prior to enabling H2O-maser emission, and possibly expand beyond a certain size before triggering OH masers.","PeriodicalId":74684,"journal":{"name":"Research notes of the AAS","volume":"70 1","pages":""},"PeriodicalIF":0.0000,"publicationDate":"2024-07-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"OH and H2O Maser Activities Among Long-period Variables\",\"authors\":\"Tian Wu and Graeme H. Smith\",\"doi\":\"10.3847/2515-5172/ad660d\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"The distribution within an infrared color–magnitude diagram of variable red giants known to have circumstellar masers is reported. Stars with H2O-maser sources occur within a color and period domain of (J − Ks) > 1.15 and P > 199 days, respectively, often in the absence of OH masers. By contrast, OH masers are mostly detected among cooler red giants with (J − Ks) > 1.35 and P > 316 days, and can coexist with H2O-maser sources. The results suggest that red giants must evolve to absolute magnitudes brighter than prior to enabling H2O-maser emission, and possibly expand beyond a certain size before triggering OH masers.\",\"PeriodicalId\":74684,\"journal\":{\"name\":\"Research notes of the AAS\",\"volume\":\"70 1\",\"pages\":\"\"},\"PeriodicalIF\":0.0000,\"publicationDate\":\"2024-07-23\",\"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/ad660d\",\"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/ad660d","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
OH and H2O Maser Activities Among Long-period Variables
The distribution within an infrared color–magnitude diagram of variable red giants known to have circumstellar masers is reported. Stars with H2O-maser sources occur within a color and period domain of (J − Ks) > 1.15 and P > 199 days, respectively, often in the absence of OH masers. By contrast, OH masers are mostly detected among cooler red giants with (J − Ks) > 1.35 and P > 316 days, and can coexist with H2O-maser sources. The results suggest that red giants must evolve to absolute magnitudes brighter than prior to enabling H2O-maser emission, and possibly expand beyond a certain size before triggering OH masers.
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