Water-maser emission from a planetary nebula with a magnetized torus

Miranda, L. F.; Gómez, Yolanda; Anglada, Guillem; Torrelles, J. M.

doi:10.1038/35104518

Cited by 119 publications

(264 citation statements)

References 22 publications

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“…The spatial distribution of the 1720 MHz OH maser spots and the presence of clear Zeeman pairs suggest that OH emission at 1720 MHz in IRAS 16333−4807 arises from an energetic ejection of material along the equatorial plane, probably in the form of an expanding, magnetized torus. Note that K 3−35, the other PN showing maser emission at 1720 MHz, has also been inferred to host a magnetized disk (Miranda et al 2001;Gómez et al 2009). These equatorial ejections could be created, for instance, by binary interactions (Nordhaus & Blackman 2006;Huggins 2007).…”

Section: The Origin Of Oh Maser Emissionmentioning

confidence: 97%

Unusual Shock-Excited Oh Maser Emission in a Young Planetary Nebula

Qiao

Walsh

Gómez

et al. 2016

ApJ

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We report on OH maser emission toward G336.644−0.695 (IRAS 16333−4807), which is a H 2 O maser-emitting Planetary Nebula (PN). We have detected 1612, 1667, and 1720 MHz OH masers at two epochs using the Australia Telescope Compact Array, hereby confirming it as the seventh known case of an OH-maser-emitting PN. This is only the second known PN showing 1720 MHz OH masers after K 3−35 and the only evolved stellar object with 1720 MHz OH masers as the strongest transition. This PN is one of a group of very young PNe. The 1612 MHz and 1667 MHz masers are at a similar velocity to the 22 GHz H 2 O masers, whereas the 1720 MHz masers show a variable spectrum, with several components spread over a higher velocity range (up to 36 km s −1 ). We also detect Zeeman splitting in the 1720 MHz transition at two epochs (with field strengths of ∼2 to ∼10 mG), which suggests the OH emission at 1720 MHz is formed in a magnetized environment. These 1720 MHz OH masers may trace short-lived equatorial ejections during the formation of the PN.

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Section: The Origin Of Oh Maser Emissionmentioning

confidence: 97%

Unusual Shock-Excited Oh Maser Emission in a Young Planetary Nebula

Qiao

Walsh

Gómez

et al. 2016

ApJ

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“…Blackman et al (2001) argue that some remnant field anchored in the core will survive even without a convection zone, although the convective envelope may not be removed completely. The idea that magnetic fields are important ingredients shaping PNe has been supported by the detection of SiO, H 2 O, and OH maser emission in circumstellar envelopes of AGB stars pointing at milliGauss fields in these nebula (Kemball & Diamond 1997;Szymczak & Cohen 1997;Miranda et al 2001;Vlemmings et al 2002Vlemmings et al , 2005Vlemmings et al , 2006Herpin et al 2006;Sabin et al 2007;Kemball et al 2009;Gómez et al 2009;Vlemmings 2011). Moreover, using an idea of Pascoli (1985), Huggins & Manley (2005) connected the extreme filamentary structures seen in high-resolution optical images of certain PNe to magnetic fields consistent with those measured in the maser from the precursor circumstellar envelopes.…”

Section: Introductionmentioning

confidence: 92%

Magnetic fields in central stars of planetary nebulae?

Jordan

Bagnulo

Werner

et al. 2012

A&A

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Context. Most planetary nebulae have bipolar or other non-spherically symmetric shapes. Magnetic fields in the central star may be responsible for this lack of symmetry, but observational studies published to date have reported contradictory results. Aims. We search for correlations between a magnetic field and departures from the spherical geometry of the envelopes of planetary nebulae. Methods. We determine the magnetic fields from spectropolarimetric observations of ten central stars of planetary nebulae. The results of the analysis of the observations of four stars were previously presented and discussed in the literature, while the observations of six stars, plus additional measurements of a star previously observed, are presented here for the first time.Results. All our determinations of magnetic field in the central planetary nebulae are consistent with null results. Our field measurements have a typical error bar of 150-300 G. Previous spurious field detections using data acquired with FORS1 (FOcal Reducer and low dispersion Spectrograph) of the Unit Telescope 1 (UT1) of the Very Large Telescope (VLT) were probably due to the use of different wavelength calibration solutions for frames obtained at different position angles of the retarder waveplate. Conclusions. There is currently no observational evidence of magnetic fields with a strength of the order of hundreds Gauss or higher in the central stars of planetary nebulae.

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“…We note that the 6035-and 1720-MHz masers lie close to the 22 GHz continuum source detected by Miranda et al (2001) (Fig. 5).…”

Section: K 3-35mentioning

confidence: 99%

Discrete Source Survey of 6 GHz OH emission from PNe and pPNe and first 6 GHz images of K 3–35

Desmurs¹,

Baudry²,

Sivagnanam³

et al. 2010

A&A

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Aims. The aim of this study is to investigate the physical properties of molecular envelopes of planetary nebulae (PNe) in their earliest stages of evolution. Methods. Using the 100 m telescope at Effelsberg, we have undertaken a high sensitivity discrete source survey for the first excited state of OH maser emission (J = 5/2, 2 Π 3/2 at 6 GHz) in the direction of PNe and proto-planetary nebulae (PNe) exhibiting 18 cm OH emission (main and/or satellite lines), and we further validate our detections using the Nançay radio telescope at 1.6-1.7 GHz and MERLIN interferometer at 1.6-1.7 and 6 GHz. Results. Two sources have been detected at 6035 MHz (5 cm), both of them are young (or very young) PNe. The first one is a confirmation of the detection of a weak 6035 MHz line in Vy 2-2. The second one is a new detection, in K 3-35, which was already known to be an exceptional late type star because it exhibits 1720 MHz OH emission. The detection of 6035 MHz OH maser emission is confirmed by subsequent observations made with the MERLIN interferometer. These lines are very rarely found in evolved stars. The 1612 MHz masers surround but are offset from the 1720 and 6035 MHz masers which in turn lie close to a compact 22 GHz continuum source embedded in the optical nebula.

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Water-maser emission from a planetary nebula with a magnetized torus

Cited by 119 publications

References 22 publications

Unusual Shock-Excited Oh Maser Emission in a Young Planetary Nebula

Unusual Shock-Excited Oh Maser Emission in a Young Planetary Nebula

Magnetic fields in central stars of planetary nebulae?

Discrete Source Survey of 6 GHz OH emission from PNe and pPNe and first 6 GHz images of K 3–35

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