Morphology and kinematics of the gas envelope of Mira Ceti

  title={Morphology and kinematics of the gas envelope of Mira Ceti},
  author={P. T. Nhung and Do T. Hoai and Pham Ngoc Diep and N. T. Phuong and Nguyen T. Thao and Pham Tuan-Anh and Pierre Darriulat},
  journal={Monthly Notices of the Royal Astronomical Society},
Observations of 12CO(3-2) emission of the circumbinary envelope of Mira Ceti, made by ALMA are analysed. The observed Doppler velocity distribution is made of three components: a blue-shifted south-eastern arc, which can be described as a ring in slow radial expansion, ~1.7 km/s, making an angle of ~50 deg with the plane of the sky and born some 2000 years ago; a few arcs, probably born at the same epoch as the blue-shifted arc, all sharing Doppler velocities red-shifted by approximately 3… 

The morpho-kinematics of the circumstellar envelope around the AGB star EP Aqr

ALMA observations of CO(1–0) and CO(2–1) emissions of the circumstellar envelope of EP Aqr, an oxygen-rich asymptotic giant branch star, are reported. A thorough analysis of their properties is

ALMA observations of the circumstellar envelope around EP Aqr

Atacama Large Millimetre/sub-millimetre Array (ALMA) observations of CO(1–0) and CO(2–1) emissions from the circumstellar envelope of the asymptotic giant branch (AGB) star EP Aqr have been made with

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Millimetre ALMA observations of the nascent winds of several Oxygen rich AGB stars have revealed the high Doppler velocity wings in their spectra. However, the physics underlying their production is

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The formation of silicate dust in oxygen-rich envelopes of evolved stars is thought to be initiated by formation of seed particles that can withstand the high temperatures close to the stellar



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Optical images and high-dispersion spectra have been obtained of the ejected material surrounding the pulsating AGB star Mira A. The two streams of knots on either side of the star, found in

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We have mapped the (CO)-C-12(3-2) line emission around the Mira AB system at 0 ''.5 resolution using the Atacama Large Millimeter/submillimeter Array (ALMA). The CO map shows amazing complexity. The

Born-Again Protoplanetary Disk around Mira B

The Mira AB system is a nearby (~107 pc) example of a wind accreting binary star system. In this class of system, the wind from a mass-losing red giant star (Mira A) is accreted onto a companion


The nature of the accreting companion to Mira—the prototypical pulsating asymptotic giant branch star—has been a matter of debate for more than 25 years. Here, we use a quantitative analysis of the

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We present K-band commissioning observations of the Mira star prototype o Cet obtained at the ESO Very Large Telescope Interferometer (VLTI) with the VINCI instrument and two siderostats. The

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Herschel’s PACS instrument observed the environment of the binary system Mira Ceti in the 70 and 160µm bands. These images reveal bright structures shaped as five broken arcs and faint er filaments

Modeling CO Emission from Mira’s Wind

We have modeled the circumstellar envelope of o Ceti (Mira) using new observational constraints. These are obtained from photospheric light scattered in near-IR vibrational-rotational lines of

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Properties of detached shells around carbon stars Evidence of interacting winds

The nature of the mechanism responsible for producing the spectacular, geometrically thin, spherical shells found around some carbon stars has been an enigma for some time. Based on extensive

First Hubble Space Telescope Observations of Mira AB Wind-accreting Binary System

The Mira AB system belongs to a class of detached binaries in which a compact object accretes mass from the wind of a cool giant or supergiant. This system provides a unique laboratory for detailed