scholarly journals Parallax of a Mira variable R Ursae Majoris studied with astrometric VLBI

2016 ◽  
Vol 68 (5) ◽  
pp. 78 ◽  
Author(s):  
Akiharu Nakagawa ◽  
Tomoharu Kurayama ◽  
Makoto Matsui ◽  
Toshihiro Omodaka ◽  
Mareki Honma ◽  
...  
Keyword(s):  
Mira Variable

scholarly journals Imaging the Surface of a Star: VLBA Monitoring of the SiO Masers around U Herculis

1998 ◽  
Vol 164 ◽  
pp. 245-246
Author(s):  
P. J. Diamond ◽  
A. J. Kemball
Keyword(s):  
Circumstellar Envelope ◽  
Mira Variable

AbstractWe report on 4 epochs of VLBA polarization observations of the 43 GHz, v=1, J=1–0 SiO masers in the circumstellar envelope around the Mira variable U Herculis.

scholarly journals Phase-referenced VLBI observations of the OH masers around U Her

1997 ◽  
Vol 180 ◽  
pp. 373-373
Author(s):  
Huib Jan Van Langevelde ◽  
James Brauher ◽  
Philip J. Diamond ◽  
Richard T. Schilizzi
Keyword(s):  
Proper Motion ◽  
Instrumental Effects ◽  
Analysis Software ◽  
Mira Variable ◽  
Vlbi Observations

We have started phase referenced monitoring of the 1667 MHz masers in the Mira variable U Her. Ultimately we hope to determine the annual parallax for this star. Three sets of VLB A observations have been performed so far. The first on July 22 1994, the second on March 6 1995 and a third on August 14 1995. Observations included bright extragalactic sources to calibrate instrumental effects and cycles of calibrator–source–calibrator (≈ 2° away) of typically 6 minutes. Without any special astrometric analysis software we detect the proper motion of U Her with an accuracy of several milli–arcseconds.

scholarly journals Rapidly Evolving Structures in the Photosphere of the Mira Variable TX Cam

2001 ◽  
Vol 205 ◽  
pp. 252-255 ◽  
Author(s):  
P. J. Diamond ◽  
A. J. Kemball
Keyword(s):  
Magnetic Field ◽  
Gravitational Field ◽  
Shock Waves ◽  
Circumstellar Envelope ◽  
Structural Variations ◽  
Mira Variable ◽  
The Magnetic Field ◽  
Dynamical Mode

44 VLBA observations of the 43 GHz SiO masers in the circumstellar envelope surrounding the Mira variable TX Cam reveal dramatic structural variations over the 80 week stellar cycle. The dominant dynamical mode is one of expansion although other complex motions are visible. The gravitational field of the star does not have a significant effect on the dynamics observed, these are probably governed more by the magnetic field and the effects of the shock waves resulting from the pulsation of the Mira itself.

Technetium in the Mira Variable RZ Pegasi

1971 ◽  
Vol 83 ◽  
pp. 496 ◽  
Author(s):  
Benjamin F., Jr. Peery ◽  
Philip C. Keenan ◽  
Irene R. Marenin
Keyword(s):  
Mira Variable
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