Book reviews

Engels, Wolf; Stützel, Thomas; Steffan, A Wilhelm; Verbeek, Bernhard

doi:10.1127/entom.gen/21/1996/117

Cited by 11 publications

(11 citation statements)

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“…The OH maser shows a typical double-peak profile, as reported in the literature such as Lewis (1994). For this source, there are two H 2 O maser observations in the literature, one by Valdettaro et al (2001) and another by Engels & Lewis (1996). Engels & Lewis (1996) observed a double-peaked profile at 37.8 and 54.8 km s −1 , which fits well with the OH maser velocity.…”

Section: Iras 19052+0922supporting

confidence: 82%

“…For this source, there are two H 2 O maser observations in the literature, one by Valdettaro et al (2001) and another by Engels & Lewis (1996). Engels & Lewis (1996) observed a double-peaked profile at 37.8 and 54.8 km s −1 , which fits well with the OH maser velocity. The H 2 O maser profile in Valdettaro et al (2001) has a single peak at 10 km s −1 .…”

Section: Iras 19052+0922supporting

confidence: 56%

“…The minimum velocity of 7.3 km s −1 given in the database was not confirmed by the H 2 O spectra in the literature. But, in the spectrum given by Engels & Lewis (1996), a weak H 2 O maser emission is detected around 27 km s −1 , implying the existence of highvelocity components on the blueshifted side. The SiO v = 1 and .…”

Section: Iras 19083+0851mentioning

confidence: 90%

“…The OH maser spectrum in Chengalur et al (1993) show three peaks at around 17, 37, and 75 km s −1 . Two H 2 O maser spectra were found in the literature (Engels & Lewis 1996;Kim et al 2013), showing strong time variation in its profile. The H 2 O maser profile is characterized by multiple peaks over a wide velocity range, similar to the profile of the known WF, IRAS 18286−0959 (Yung et al 2011).…”

Section: Iras 19083+0851mentioning

confidence: 90%

“…The H 2 O maser profile in Valdettaro et al (2001) has a single peak at 10 km s −1 . The 10 km s −1 peak of Valdettaro et al (2001) was apparently not present in the spectra of Engels & Lewis (1996). The 10 km s −1 peak is clearly outside the velocity range of the OH maser line (the peak velocity of the OH redshifted component is near 26 km s −1 ).…”

Section: Iras 19052+0922mentioning

confidence: 91%

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Systematic Search for Water Fountain Candidates Using the Databases of Circumstellar Maser Sources

Fan 范,

Nakashima 中岛,

Engels

et al. 2024

ApJS

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Water fountains (WFs) are thought to be objects in the morphological evolution of the circumstellar envelopes of low- and intermediate-mass evolved stars, transitioning from spherically symmetric to asymmetric shapes. We used databases of circumstellar 1612 MHz OH and 22.235 GHz H2O maser sources to search for new WF candidates using the criterion of a larger velocity range of the H2O maser emission compared to that of the OH maser emission. Thus, it is in principle possible to identify WFs with H2O velocity ranges smaller than those for the previously known WFs. For the OH maser line, we analyzed database entries of 8474 observations from 2195 sources, and 6085 observations from 3642 sources for the H2O maser line. After a close examination of the velocity ranges and line profiles, we identified 11 sources that meet the criterion mentioned above. We examined the IRAS colors of the selected sources and found that two of them (IRAS 19069+0916 and IRAS 19319+2214) are in the color region for post-AGB stars. We find that the maser velocity criterion can discover other astrophysically interesting objects than just WFs. Such objects may include peculiar planetary nebulae with maser emissions and stellar merger remnants.

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Section: Iras 19052+0922supporting

confidence: 82%

Section: Iras 19052+0922supporting

confidence: 56%

Section: Iras 19083+0851mentioning

confidence: 90%

Section: Iras 19083+0851mentioning

confidence: 90%

Section: Iras 19052+0922mentioning

confidence: 91%

See 3 more Smart Citations

Systematic Search for Water Fountain Candidates Using the Databases of Circumstellar Maser Sources

Fan 范,

Nakashima 中岛,

Engels

et al. 2024

ApJS

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Near IR Observations of the Arecibo Sample of OH/IR Stars

Jiménez-Esteban

Engels

García-Lario³

2001

Post-Agb Objects as a Phase of Stellar Evolution

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We performed a near-IR/optical monitoring programme from 1999 to 2005 in order to study the variability properties of the 'Arecibo sample of OH/IR stars' (periods, amplitudes, and colour variations). Here we describe this multiwavelength long-term monitoring programme. Data analysis is still in process. Our ultimate goal is to study in particular the oxygen-rich AGB stars with M > 2 M ⊙ , which are probably rare among AGB stars discovered optically and/or in the near-IR, but are common in samples discovered in the mid-to far-IR.

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Mass Loss in Evolved Stars

Matthews

2022

Proc. IAU

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Intense mass loss through cool, low-velocity winds is a defining characteristic of low-to-intermediate mass stars during the asymptotic giant branch (AGB) evolutionary stage. Such winds return up ∼80% of the initial stellar mass to the interstellar medium and play a major role in enriching it with dust and heavy elements. A challenge to understanding the physics underlying AGB mass loss is its dependence on an interplay between complex and highly dynamic processes, including pulsations, convective flows, shocks, magnetic fields, and opacity changes resulting from dust and molecule formation. I highlight some examples of recent advances in our understanding of late-stage stellar mass loss that are emerging from radio and (sub)millimeter observations, with a particular focus on those that resolve the surfaces and extended atmospheres of evolved stars in space, time, and frequency.

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Book reviews

Cited by 11 publications

References 0 publications

Systematic Search for Water Fountain Candidates Using the Databases of Circumstellar Maser Sources

Systematic Search for Water Fountain Candidates Using the Databases of Circumstellar Maser Sources

Near IR Observations of the Arecibo Sample of OH/IR Stars

Mass Loss in Evolved Stars

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