The Proto–Planetary Nebula M1‐92 and the Symbiotic Star MWC 560: Two Evolutionary Phases of the Same Type of Object?

Arrieta, A.; Torres-Peimbert, S.; Георгиев, Л.

doi:10.1086/428391

Cited by 18 publications

(28 citation statements)

References 30 publications

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“…Bujarrabal et al (1998b) estimated that the mass of the ionized gas in the nebula is only about 10 −3 M , and Arrieta et al (2005) concluded that the present ionized mass loss is very low, 3 × 10 −13 M yr −1 .…”

Section: Introductionmentioning

confidence: 93%

“…The central star has a spectrum compatible with T eff = 6500 K and log g = 0.5, although at short wavelengths it shows an excess that can be fitted with the presence of a secondary star of T eff = 18 000 K and log g = 5.0 (Arrieta et al 2005). The distance to M 1-92 has been estimated as 2.5 kpc, adopting a nominal luminosity of 10 4 L for a post-AGB star (Cohen & Kuhi 1977).…”

Section: Introductionmentioning

confidence: 99%

“…This axis is inclined in respect to the plane of the sky by about 35 • , with the northwest lobe pointing to us. Optical spectroscopy shows the presence of wide absorption components, revealing the existence of (bipolar) flows of ionized gas close to the star, with expansion velocities up to 750 km s −1 (Arrieta et al 2005). Line emission in Hα and in atomic forbidden lines (O i, O iii, N ii, S ii) is detected from the middle of the two lobes (Bujarrabal et al 1998b), Based on observations carried out with the IRAM Plateau de Bure Interferometer.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Minkowski's footprint revisited

Alcolea¹,

Neri

Bujarrabal

2007

A&A

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Context. M 1-92 can be considered an archetype of bipolar pre-planetary nebulae. It shows a clear axial symmetry, along with the kinematics and momentum excess characteristic of this class of envelopes around post-AGB stars. Aims. By taking advantage of the new extended configuration of the IRAM Plateau de Bure interferometer, we wanted to study the morphology and velocity field of the molecular gas better in this nebula, particularly in its central part.Methods. We performed sub-arcsecond resolution interferometric observations of the J = 2−1 rotational line of 13 CO in M 1-92. Results. We found that the equatorial component is a thin flat disk, which expands radially with a velocity proportional to the distance to the center. The kinetic age of this equatorial flow is very similar to that of the two lobes. The small widths and velocity dispersion in the gas forming the lobe walls confirm that the acceleration responsible for the nebular shape could not last more than 100-120 yr.Conclusions. The present kinematics of the molecular gas can be explained as the result of a single brief acceleration event, after which the nebula reached an expansion velocity field with axial symmetry. In view of the similarity to other objects, we speculate on the possibility that the whole nebula was formed as a result of a magneto-rotational explosion in a common-envelope system.

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Section: Introductionmentioning

confidence: 93%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Minkowski's footprint revisited

Alcolea¹,

Neri

Bujarrabal

2007

A&A

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“…It is difficult to include jets in either the hydrodynamic calculations because of the supersonic velocities, or the radiative transfer calculations. Nevertheless, the possibility of a jet contribution to either Hα and Hβ formation has been demonstrated by several studies (Budaj & Richards 2004;Arrieta et al 2005). …”

Section: Jet Launching In the Accretion Disk Of The Companionmentioning

confidence: 99%

Time-resolved spectroscopy of BD+46°442: Gas streams and jet creation in a newly discovered evolved binary with a disk

Gorlova

Winckel

Gielen

et al. 2012

A&A

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Context. Previous studies have shown that many post-asymptotic giant branch (AGB) stars with dusty disks are associated with single-lined binary stars. The inferred orbital separations are too small to accommodate a fully grown AGB star, hence these systems represent a new evolutionary channel that bypasses a full AGB evolution. Aims. We wish to verify the binarity hypothesis for a larger sample establish the nature of the companions, and probe the disk structure and eventually the disk formation mechanisms in binary stars. To achieve these aims, we started a high-resolution spectral monitoring of ∼40 field giants whose binarity had been suspected based on either a light curve, an infrared excess, or a peculiar chemical composition. Methods. Starting from the spring of 2009, we monitored the programme stars with the fibre echelle spectrometer HERMES. We measure their radial velocities (RVs) with a precision of ∼0.2 km s −1 , perform detailed photospheric abundance analyses, and analyse the time-resolved high-resolution spectra to search for line-profile variability.Results. Here we report on the discovery of periodic RV variations in BD+46 • 442, a high Galactic latitude F giant with a disk. We infer that the variations are caused by the motion around a faint companion, and deduce the orbital parameters P orb = 140.77 ± 0.02 d , e = 0.083± 0.002, and a sin i = 0.31 AU. We find that it is a moderately metal-poor star ([M/H] = −0.7) without a strong depletion pattern in its photospheric abundances. Interestingly, many lines indeed show periodic changes with the orbital phase: Hα switches between a double-peak emission line and a P Cyg-like profile, while strong metal lines appear to be split at the maximum redshift. Similar effects are likely visible in the spectra of other post-AGB binaries, but their regularity is not always apparent owing to sporadic observations. We propose that these features result from an ongoing mass transfer from the evolved giant to the companion. In particular, the blueshifted absorption in Hα, which occurs only at superior conjunction, may result from a jet originating in the accretion disk around the companion and that is seen in absorption towards the luminous primary.

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“…Many new observations and theoretical studies since the turn of the Millennium further consolidated the jet-shaping scenario of many PNe (e.g., Parthasarathy et al 2000;Bujarrabal et al 2001;Miranda et al 2001;Corradi et al 2001b;Guerrero et al 2001;Imai et al 2002;Riera et al 2003;Vinković et al 2004;Huggins et al 2004;Peña et al 2004;Balick & Hajian 2004;Arrieta et al 2005;Oppenheimer et al 2005;Sahai et al 2005;Vlemmings et al 2006;Miranda et al 2010;Nakashima et al 2010;Phillips et al 2010;Sahai et al 2011;Szyszka et al 2011;López et al 2012;Clark et al 2013;Pérez-Sánchez et al 2013;Vlemmings et al 2014;Fang et al 2015 Dennis et al 2008Dennis et al , 2009Lee et al 2009;Huarte-Espinosa et al 2012;Velázquez et al 2012;Balick et al 2013;Velázquez et al 2014 for theoretical studies; these papers composed a small fraction of the papers studying jets in PNe). X-ray observations seem also to support the presence of jet-inflated bubbles and of jets Sahai et al 2003), similar to X-ray jets in symbiotic systems (e.g., Kellogg et al 2001;Galloway & Sokoloski 2004).…”

Section: Pn Morphologiesmentioning

confidence: 99%

The jet feedback mechanism (JFM) in stars, galaxies and clusters

Soker

2016

New Astronomy Reviews

149

106

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I review the influence jets and the bubbles they inflate might have on their ambient gas as they operate through a negative jet feedback mechanism (JFM). I discuss astrophysical systems where jets are observed to influence the ambient gas, in many cases by inflating large, hot, and low-density bubbles, and systems where the operation of the JFM is still a theoretical suggestion. The first group includes cooling flows in galaxies and clusters of galaxies, star-forming galaxies, young stellar objects, and bipolar planetary nebulae. The second group includes core collapse supernovae, the common envelope evolution, the grazing envelope evolution, and intermediate luminosity optical transients. The suggestion that the JFM operates in these four types of systems is based on the assumption that jets are much more common than what is inferred from objects where they are directly observed. Common to all eight types of systems reviewed here is the presence of a compact object inside an extended ambient gas. The ambient gas serves as a potential reservoir of mass to be accreted on to the compact object. If the compact object launches jets as it accretes mass, the jets might reduce the accretion rate as they deposit energy to the ambient gas, or even remove the entire ambient gas, hence closing a negative feedback cycle.

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The Proto–Planetary Nebula M1‐92 and the Symbiotic Star MWC 560: Two Evolutionary Phases of the Same Type of Object?

Cited by 18 publications

References 30 publications

Minkowski's footprint revisited

Minkowski's footprint revisited

Time-resolved spectroscopy of BD+46°442: Gas streams and jet creation in a newly discovered evolved binary with a disk

The jet feedback mechanism (JFM) in stars, galaxies and clusters

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