On the magnetic field of OH 231.8+4.2

Marcelo L. Leal-Ferreira; Wouter H.T. Vlemmings; Philip J. Diamond; Athol Kemball; Nikta Amiri; Jean François Desmurs

doi:10.1017/S1743921312011714

On the magnetic field of OH 231.8+4.2

Marcelo L. Leal-Ferreira, Wouter H.T. Vlemmings, Philip J. Diamond, Athol Kemball, Nikta Amiri, Jean François Desmurs

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

Abstract

During the transition from an AGB star to a planetary nebula, a large number of low/intermediate initial mass stars loses its spherical symmetry. The process responsible for that change of morphology is, so far, not well understood. The candidates responsible for shaping these objects are (i) a companion to the star (binary/heavy planet) and its tidal forces, (ii) disk interaction and (iii) magnetic fields - or a combination of these. In particular a binary induced magnetic field is a promising option. To study this we observed the polarization of H₂O masers in the known binary pre-Planetary Nebula (pPN) OH231.8+4.2. Our results show a magnetic field B _|| of ∼45 mG is present in the H₂O maser region of this pPN.

Original language	English (US)
Title of host publication	Planetary Nebulae
Subtitle of host publication	An Eye to the Future
Pages	418-419
Number of pages	2
Edition	S283
DOIs	https://doi.org/10.1017/S1743921312011714
State	Published - Jul 2011

Publication series

Name	Proceedings of the International Astronomical Union
Number	S283
Volume	7
ISSN (Print)	1743-9213
ISSN (Electronic)	1743-9221

Keywords

magnetic fields
masers
polarization
stars: AGB and post-AGB
stars: individual (OH231.8+4.2)

ASJC Scopus subject areas

Medicine (miscellaneous)
Astronomy and Astrophysics
Nutrition and Dietetics
Public Health, Environmental and Occupational Health
Space and Planetary Science

Online availability

10.1017/S1743921312011714

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title = "On the magnetic field of OH 231.8+4.2",

abstract = "During the transition from an AGB star to a planetary nebula, a large number of low/intermediate initial mass stars loses its spherical symmetry. The process responsible for that change of morphology is, so far, not well understood. The candidates responsible for shaping these objects are (i) a companion to the star (binary/heavy planet) and its tidal forces, (ii) disk interaction and (iii) magnetic fields - or a combination of these. In particular a binary induced magnetic field is a promising option. To study this we observed the polarization of H2O masers in the known binary pre-Planetary Nebula (pPN) OH231.8+4.2. Our results show a magnetic field B || of ∼45 mG is present in the H2O maser region of this pPN.",

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author = "Leal-Ferreira, {Marcelo L.} and Vlemmings, {Wouter H.T.} and Diamond, {Philip J.} and Athol Kemball and Nikta Amiri and Desmurs, {Jean Fran{\c c}ois}",

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AU - Leal-Ferreira, Marcelo L.

AU - Vlemmings, Wouter H.T.

AU - Diamond, Philip J.

AU - Kemball, Athol

AU - Amiri, Nikta

AU - Desmurs, Jean François

PY - 2011/7

Y1 - 2011/7

N2 - During the transition from an AGB star to a planetary nebula, a large number of low/intermediate initial mass stars loses its spherical symmetry. The process responsible for that change of morphology is, so far, not well understood. The candidates responsible for shaping these objects are (i) a companion to the star (binary/heavy planet) and its tidal forces, (ii) disk interaction and (iii) magnetic fields - or a combination of these. In particular a binary induced magnetic field is a promising option. To study this we observed the polarization of H2O masers in the known binary pre-Planetary Nebula (pPN) OH231.8+4.2. Our results show a magnetic field B || of ∼45 mG is present in the H2O maser region of this pPN.

AB - During the transition from an AGB star to a planetary nebula, a large number of low/intermediate initial mass stars loses its spherical symmetry. The process responsible for that change of morphology is, so far, not well understood. The candidates responsible for shaping these objects are (i) a companion to the star (binary/heavy planet) and its tidal forces, (ii) disk interaction and (iii) magnetic fields - or a combination of these. In particular a binary induced magnetic field is a promising option. To study this we observed the polarization of H2O masers in the known binary pre-Planetary Nebula (pPN) OH231.8+4.2. Our results show a magnetic field B || of ∼45 mG is present in the H2O maser region of this pPN.

KW - magnetic fields

KW - masers

KW - polarization

KW - stars: AGB and post-AGB

KW - stars: individual (OH231.8+4.2)

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DO - 10.1017/S1743921312011714

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T3 - Proceedings of the International Astronomical Union

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BT - Planetary Nebulae

ER -

On the magnetic field of OH 231.8+4.2

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