R. Abuter, M. Accardo, T. Adler, A. Amorim, N. Anugu, G. Ávila, M. Bauböck, M. Benisty, J. Berger, J. Bestenlehner, H. Beust, N. Blind, M. Bonnefoy, H. Bonnet, P. Bourget, J. Bouvier, W. Brandner, R. Brast, A. Buron, L. Burtscher, F. Cantalloube, A. C. O. Garatti, P. Caselli, F. Cassaing, F. Chapron, B. Charnay, É. Choquet, Y. Clénet, C. Collin, V. C. Foresto, R. Davies, C. Deen, F. Delplancke-Ströbele, R. Dembet, F. Dérie, W. D. Wit, J. Dexter, T. Zeeuw, C. Dougados, G. Dubus, G. Duvert, M. Ebert, A. Eckart, F. Eisenhauer, M. Esselborn, F. Eupen, P. Fédou, M. Ferreira, G. Finger, N. F. Schreiber, F. Gao, C. G. Dabo, R. G. López, P. Garcia, E. Gendron, R. Genzel, O. Gerhard, J. Gil, S. Gillessen, F. Gonté, P. Gordo, D. Gratadour, A. Greenbaum, R. Grellmann, U. Grözinger, P. Guajardo, S. Guieu, M. Habibi, P. Haguenauer, O. Hans, X. Haubois, M. Haug, F. Haussmann, T. Henning, S. Hippler, S. Hönig, M. Horrobin, A. Huber, Z. Hubert, N. Hubin, C. Hummel, G. Jakob, A. Janssen, A. Rosales, L. Jochum, L. Jocou, J
{"title":"利用CO - ro振动发射对赫比格51星内部气体盘的空间解析","authors":"R. Abuter, M. Accardo, T. Adler, A. Amorim, N. Anugu, G. Ávila, M. Bauböck, M. Benisty, J. Berger, J. Bestenlehner, H. Beust, N. Blind, M. Bonnefoy, H. Bonnet, P. Bourget, J. Bouvier, W. Brandner, R. Brast, A. Buron, L. Burtscher, F. Cantalloube, A. C. O. Garatti, P. Caselli, F. Cassaing, F. Chapron, B. Charnay, É. Choquet, Y. Clénet, C. Collin, V. C. Foresto, R. Davies, C. Deen, F. Delplancke-Ströbele, R. Dembet, F. Dérie, W. D. Wit, J. Dexter, T. Zeeuw, C. Dougados, G. Dubus, G. Duvert, M. Ebert, A. Eckart, F. Eisenhauer, M. Esselborn, F. Eupen, P. Fédou, M. Ferreira, G. Finger, N. F. Schreiber, F. Gao, C. G. Dabo, R. G. López, P. Garcia, E. Gendron, R. Genzel, O. Gerhard, J. Gil, S. Gillessen, F. Gonté, P. Gordo, D. Gratadour, A. Greenbaum, R. Grellmann, U. Grözinger, P. Guajardo, S. Guieu, M. Habibi, P. Haguenauer, O. Hans, X. Haubois, M. Haug, F. Haussmann, T. Henning, S. Hippler, S. Hönig, M. Horrobin, A. Huber, Z. Hubert, N. Hubin, C. Hummel, G. Jakob, A. Janssen, A. Rosales, L. Jochum, L. Jocou, J","doi":"10.18727/0722-6691/5174","DOIUrl":null,"url":null,"abstract":"1 GRAVITY operates in the near-infrared K-band, i.e., with wavelengths between 2 and 2.5 μm. 2 PIONIER at the VLTI operates in the near-infrared H-band, i.e., with wavelengths between 1.5 and 1.8 μm. 3 MATISSE at the VLTI operates in the mid-infrared L-, M-, and N-bands, i.e., with wavelengths between 3 and 13 μm (Lopez et al., 2018). emission we measured with GRAVITY is located at positions smaller than the critical radius where the gap is expected to form as a result of to extreme-/farultraviolet/X-ray heating, the discs in our sample might be shaped by forming young planets rather than by depletion resulting from photoevaporation (Figure 2).","PeriodicalId":41738,"journal":{"name":"Jurnal The Messenger","volume":"19 1","pages":"40-42"},"PeriodicalIF":0.3000,"publicationDate":"2019-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"Spatially Resolving the Inner Gaseous Disc of the Herbig Star 51 Oph through its CO Ro-vibration Emission\",\"authors\":\"R. Abuter, M. Accardo, T. Adler, A. Amorim, N. Anugu, G. Ávila, M. Bauböck, M. Benisty, J. Berger, J. Bestenlehner, H. Beust, N. Blind, M. Bonnefoy, H. Bonnet, P. Bourget, J. Bouvier, W. Brandner, R. Brast, A. Buron, L. Burtscher, F. Cantalloube, A. C. O. Garatti, P. Caselli, F. Cassaing, F. Chapron, B. Charnay, É. Choquet, Y. Clénet, C. Collin, V. C. Foresto, R. Davies, C. Deen, F. Delplancke-Ströbele, R. Dembet, F. Dérie, W. D. Wit, J. Dexter, T. Zeeuw, C. Dougados, G. Dubus, G. Duvert, M. Ebert, A. Eckart, F. Eisenhauer, M. Esselborn, F. Eupen, P. Fédou, M. Ferreira, G. Finger, N. F. Schreiber, F. Gao, C. G. Dabo, R. G. López, P. Garcia, E. Gendron, R. Genzel, O. Gerhard, J. Gil, S. Gillessen, F. Gonté, P. Gordo, D. Gratadour, A. Greenbaum, R. Grellmann, U. Grözinger, P. Guajardo, S. Guieu, M. Habibi, P. Haguenauer, O. Hans, X. Haubois, M. Haug, F. Haussmann, T. Henning, S. Hippler, S. Hönig, M. Horrobin, A. Huber, Z. Hubert, N. Hubin, C. Hummel, G. Jakob, A. Janssen, A. Rosales, L. Jochum, L. Jocou, J\",\"doi\":\"10.18727/0722-6691/5174\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"1 GRAVITY operates in the near-infrared K-band, i.e., with wavelengths between 2 and 2.5 μm. 2 PIONIER at the VLTI operates in the near-infrared H-band, i.e., with wavelengths between 1.5 and 1.8 μm. 3 MATISSE at the VLTI operates in the mid-infrared L-, M-, and N-bands, i.e., with wavelengths between 3 and 13 μm (Lopez et al., 2018). emission we measured with GRAVITY is located at positions smaller than the critical radius where the gap is expected to form as a result of to extreme-/farultraviolet/X-ray heating, the discs in our sample might be shaped by forming young planets rather than by depletion resulting from photoevaporation (Figure 2).\",\"PeriodicalId\":41738,\"journal\":{\"name\":\"Jurnal The Messenger\",\"volume\":\"19 1\",\"pages\":\"40-42\"},\"PeriodicalIF\":0.3000,\"publicationDate\":\"2019-12-01\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Jurnal The Messenger\",\"FirstCategoryId\":\"1085\",\"ListUrlMain\":\"https://doi.org/10.18727/0722-6691/5174\",\"RegionNum\":0,\"RegionCategory\":null,\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"Q4\",\"JCRName\":\"COMMUNICATION\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"Jurnal The Messenger","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.18727/0722-6691/5174","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q4","JCRName":"COMMUNICATION","Score":null,"Total":0}
Spatially Resolving the Inner Gaseous Disc of the Herbig Star 51 Oph through its CO Ro-vibration Emission
1 GRAVITY operates in the near-infrared K-band, i.e., with wavelengths between 2 and 2.5 μm. 2 PIONIER at the VLTI operates in the near-infrared H-band, i.e., with wavelengths between 1.5 and 1.8 μm. 3 MATISSE at the VLTI operates in the mid-infrared L-, M-, and N-bands, i.e., with wavelengths between 3 and 13 μm (Lopez et al., 2018). emission we measured with GRAVITY is located at positions smaller than the critical radius where the gap is expected to form as a result of to extreme-/farultraviolet/X-ray heating, the discs in our sample might be shaped by forming young planets rather than by depletion resulting from photoevaporation (Figure 2).
求助内容：
应助结果提醒方式：
京公网安备 11010802042870号
