Many people have written to describe data that contain negative values and to ask for advice about how to log-transform the data. Into the inner disk, either in the plane of the bulk of the disk material or inĪ slightly inclined (non-coplanar) orbit.In my four years of blogging, the post that has generated the most comments is "How to handle negative values in log transformations." We propose that these deviations mightīe indicative of the injection (and subsequent circularization) of new blobs Polarization position angle during polarization outbursts in each star, We also observe deviations from the mean intrinsic Suggesting that the outbursts represent the injection and subsequent viscousĭissipation of individual blobs of material into the inner circumstellarĮnvironments of these stars.
Star shared similar lifetimes as those previously reported for mu Cen, Minor outbursts observed during the quiescent phase of each Intrinsic polarization to be 166.7 +/- 0.1 degrees for pi Aqr and 107.7 +/- 0.4ĭegrees for 60 Cyg, and model the observed polarization during the quiescentĭiskless phase of each star to determine the interstellar polarization along The polarization and H-alpha in both stars indicates the disk clearing An observed time lag between the behavior of
pi Aqr's disk loss was episodic in nature and occurred Time-scale of 1000 days, consistent with the viscous time-scale of the disk,Īssuming alpha is 0.14. 60 Cyg's disk lossĮpisode was characterized by a monotonic decrease in emission strength over a Such a transition for two Be stars, pi Aquarii and 60 Cygni. We present one of the most comprehensive spectropolarimetric views to date of Kowalski (1) ((1) University of Washington, (2) University of Toledo, (3) University of Wisconsin) Download PDF Abstract: (Abridged) Classical Be stars occasionally transition from having a gaseousĬircumstellar disk (''Be phase'') to a state in which all observationalĮvidence for the presence of these disks disappears (''normal B-star phase'').
0 kommentar(er)
