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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >VLBI Monitoring Observations of Water Masers around the Semi-Regular Variable Star R Crateris
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VLBI Monitoring Observations of Water Masers around the Semi-Regular Variable Star R Crateris

机译：VLBI监测半规则变星R Crateris附近水质的观测

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Wemonitoredwater-vapormasersaroundthesemi-regularvariablestarRCrateriswiththeJapaneseVLBINetwork(J-Net)atthe22GHzbandduringfourepochswithintervalsofonemonth.TherelativepropermotionsandDoppler-velocitydriftsoftwelvemaserfeaturesweremeasured.Mostofthemexistedforlongerthan80days.The3-Dkinematicsofthefeaturesindicatesabipolarexpandingflow.ThemajoraxisoftheasymmetricflowwasestimatedtobeatP.A.$$=136^{circ}$$.TheexistenceofabipolaroutflowsuggeststhataMiravariablestarhadalreadyformedabipolaroutflow.Thewatermasersareinaregionofapparentminimumradiiof$$1.3 imes10^{12},mathrm{m}$$andmaximumradiiof$$2.6 imes10^{12},mathrm{m}$$,betweenwhichtheexpansionvelocityrangesfrom4.3to$$7.4,mathrm{km},mathrm{s}^{-1}$$.Thesevaluessuggestthatthewatermasersareradiallyaccelerated,butstillgravitationallybound,inthewater-maserregion.Themostpositiveandnegativevelocity-driftingfeatureswerefoundrelativelyclosetothesystemicvelocityofthestar.Wefoundthattheblue-shiftedfeaturesareapparentlyacceleratedandthered-shiftedapparentlydecelerated.Theaccelerationofonlytheblue-shiftedfeaturesseemstobeconsistentwiththatoftheexpandingflowfromthestar.
机译：Wemonitoredwater-vapormasersaroundthesemi-regularvariablestarRCrateriswiththeJapaneseVLBINetwork（J-净）atthe22GHzbandduringfourepochswithintervalsofonemonth.TherelativepropermotionsandDoppler-velocitydriftsoftwelvemaserfeaturesweremeasured.Mostofthemexistedforlongerthan80days.The3-Dkinematicsofthefeaturesindicatesabipolarexpandingflow.ThemajoraxisoftheasymmetricflowwasestimatedtobeatP.A。$$ = 136 ^ {} CIRC $$。TheexistenceofabipolaroutflowsuggeststhataMiravariablestarhadalreadyformedab​​ipolaroutflow.Thewatermasersareinaregionofapparentminimumradiiof $$ 1.3 imes10 ^ {12}，{mathrm m} $$和$ 2.6的最大半径，imes10 ^ {12}，mathrm {m} $$，两者之间的扩展速度在4.3到$$ 7.4之间，mathrm {km}，mathrm {s} ^ {-1} $$。相对于恒星的系统速度，发现了最正负的速度漂移特征。我们发现，蓝移特征明显加速并且变位了。请注意，只有蓝移特征的加速度才与恒星不断膨胀的加速度一致。

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