Central Bureau for Astronomical Telegrams
IAUC 5151: COORDINATED Obs OF MIRA AB AND R Leo; MWC 560
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Read IAUC 5152
Circular No. 5151
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
Telephone 617-495-7244/7440/7444 (for emergency use only)
TWX 710-320-6842 ASTROGRAM CAM EASYLINK 62794505
MARSDEN or GREEN@CFA.BITNET MARSDEN or GREEN@CFAPS2.SPAN
COORDINATED OBSERVATIONS OF MIRA AB AND R LEONIS
M. Karovska and E. Guinan communicate: "As part of the ongoing
campaign of coordinated observations (cf. IAUC 5043) of the detached
binary system Mira (omicron Ceti) AB, ground-based speckle interferometry
observations will be obtained during 1991 Jan. 3-7 and Jan.
29-Feb. 7. Mira AB will also be observed from space with the IUE
satellite on Jan. 15 and 29 and Feb. 7, and with ROSAT on Jan. 15.
The major objectives of these observations are to study the effects
of stellar pulsation on the extended atmosphere of Mira A (the
prototype of Mira variables) and to study in detail the accretion
processes in detached binaries. We will extend our ground-based
observations to R Leo, which is a nearby Mira variable very similar to
Mira A. To optimize this observing opportunity, we solicit coordinated,
near-simultaneous ground-based photometric (especially intermediate-band
photometry), polarimetric, spectroscopic, infrared, and
radio observations of the Mira system and R Leo. In January and the
beginning of February, Mira A will be at phase 0.3-0.4 of its
lightcurve, and R Leo will be near maximum light. Those interested in
participating in the observing campaign should contact M. Karovska
(Center for Astrophysics, 60 Garden St., Cambridge, MA 02138,
U.S.A,; telephone 617-495-7347; e-mail KAROVSKA@CFA.BITNET or
GUINAN@VUVAXCOM)."
MWC 560
B. W. Bopp, University of Toledo, writes: "Spectroscopic
observations of the unusual emission-line object MWC 560 were obtained
at Ritter Observatory on Nov. 30 and Dec. 1 UT. CCD scans (range
590-680 and 820-910 nm, resolution 0.2 nm) show a narrow, intense H-
alpha emission line with a P-Cyg absorption component shifted by
-500 km/s. There are numerous narrow emission features of Fe II
(multiplets 40 and 74) present between 600 and 650 nm, along with
weak [O I] 630.0-nm and He I 667.8-nm emission lines. In the 820-
to 910-nm region, the Ca II infrared triplet lines are seen strongly
in emission, superimposed on the continuum of a red star. TiO
bandheads at 846, 886, and 894 nm are prominent and infer a spectral
type near M5. MWC 560 was observed for several hours, and several
spectra with 20-min time resolution were obtained, but no
significant changes in line profiles or intensity were seen."
1990 December 26 (5151) Daniel W. E. Green
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