Results 211 to 220 of about 411 (243)

A whole-animal phenotypic drug screen identifies suppressors of atherogenic lipoproteins. [PDF]

Elife
Kelpsch DJ, Zhang L, Thierer JH, Rivera Cruz AG, Koren K, Kumar U, Lin Y, Hensley MR, Sohn M, Liu JO, Lectka T, Mumm JS, Farber SA.   +12 more
europepmc   +1 more source

Fitness seascapes are necessary for realistic modeling of the evolutionary response to drug therapy. [PDF]

Sci Adv
King ES, Stacy AE, Weaver DT, Maltas J, Barker-Clarke R, Dolson E, Scott JG.   +6 more
europepmc   +1 more source

OH emission from Mira variables, infrared stars and molecular clouds

, 1985
Slootmaker, A., Habing, H.J., Herman, J.
openaire   +1 more source

Further VLBA Observations of SiO Masers Toward Mira Variable Stars [PDF]

Astronomy and Astrophysics, 2006
We present the results of continued monitoring of the SiO masers at 7 mm wavelength in several of the Mira variable stars reported in Cotton et al. (2004, A&A, 414, 275) (o Ceti = Mira, U Orionis = U Ori, R Aquarii = R Aqr) over a period of 16 months, extending the observations to several pulsation cycles. The observed size of the maser rings varied by
Wouter Vlemmings, P J Diamond, W D Cotton   +2 more
exaly   +5 more sources

VLBA Observations of SiO Masers Towards Mira Variable Stars [PDF]

Astronomy and Astrophysics, 2004
We present new total intensity and linear polarization VLB A observations of the v = 2 and v = 1 J = 1-0 maser transitions of SiO at 42.8 and 43.1 GHz in a number of Mira variable stars over a substantial fraction of their pulsation periods. These observations were part of an observing program that also includes interferometric measurements at 2.2 and ...
Wouter Vlemmings, P J Diamond, S Morel
exaly   +4 more sources

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A problem in distance-determination for Mira variables with an appendix on OB-star distances

Vistas in Astronomy, 1972
Abstract Difficulties in accepting the results on the kinematics of distant Mira variables obtained by Smak and Preston (1965) and in paper II, are outlined. It is shown that proper allowance for statistical bias in the distance determinations together with an allowance for the different definition of maximum magnitude, as used in these two ...
openaire   +1 more source

Optical Interferometry and Mira Variable Stars

2005
This thesis describes the development of a red tip/tilt and fringe detection system at the Sydney University Stellar Interferometer (SUSI), modelling the instrumental performance and effects of seeing at SUSI, making observations of Mira variable stars and finally modelling the atmospheres of Mira variables with physically self-consistent models.
openaire   +1 more source

Spectral Analyses of Some Mira-Type Long-Period Variable Stars

Publications of the Astronomical Society of Japan, 1971
Abstract Spectral analyses were made for the spectrograms obtained near the light maximum of seven Mira-type long-period variable stars: χ Cygni, o Ceti, R Leonis, R Hydrae, R Trianguli, T Ursae Majoris, and R Cassiopeiae. For each spectrogram, identifications of spectral lines were made, and equivalent widths were measured. It was found
openaire   +1 more source

Optical and infrared aperture masking interferometry of mira variable stars

2009
1.1 A Brief History of Interferometry The theoretical angular resolution of a telescope with perfect optics is proportional to the diameter of the aperture. A 10 m telescope (e.g. the Keck I telescope on Mauna Kea, Hawaii) in the visible range of light (x1 z 500 nm) could theoretically achieve resolutions of 12 milliarcseconds (mas). It might seem that
openaire   +1 more source

5.1.2.6 Mira stars (long period variables) - M

2005
H. W. Duerbeck, W. C. Seitter
openaire   +1 more source