NEW MEASUREMENTS OF THE RADIO PHOTOSPHERE OF MIRA BASED ON DATA FROM THE JVLA AND ALMA

• Main Authors: Reid, M. J. (Author), Menten, K. M. (Author), Matthews, Lynn D. (Contributor)
• Other Authors: Haystack Observatory (Contributor)
• Format: Article
• Language: English
• Published: IOP Publishing, 2015-09-03T16:43:19Z.
• Subjects: Article
• Online Access: Get fulltext

 We present new measurements of the millimeter wavelength continuum emission from the long period variable Mira (o Ceti) at frequencies of 46, 96, and 229 GHz (λ ≈ 7, 3, and 1 mm) based on observations obtained with the Jansky Very Large Array (JVLA) and the Atacama Large Millimeter/submillimeter Array (ALMA). The measured millimeter flux densities are consistent with a radio photosphere model derived from previous observations, where flux density S[subscript ν] ∝ ν[superscript 1.86]. The stellar disk is resolved, and the measurements indicate a decrease in the size of the radio photosphere at higher frequencies, as expected if the opacity decreases at shorter wavelengths. The shape of the radio photosphere is found to be slightly elongated, with a flattening of ~10%-20%. The data also reveal evidence for brightness non-uniformities on the surface of Mira at radio wavelengths. Mira's hot companion, Mira B was detected at all three observed wavelengths, and we measure a radius for its radio-emitting surface of ≈2.0 X 10[superscript 13] cm. The data presented here highlight the power of the JVLA and ALMA for the study of the atmospheres of evolved stars.