The peculiar object He 2-467.

Lutz, J. H.; Lutz, T. E.; Kaler, J. B.; Osterbrock, Donald E.; Gregory, S. A.

doi:10.1086/154102

Cited by 14 publications

(21 citation statements)

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“…The variation between these two dates for F(A4686)/H/? is similar to the variation initially detected by Lutz (1977).…”

Section: Resultssupporting

confidence: 88%

“…The entire set of filters was used on only one night, 1978 September 18, JD'770. On this night the data were reduced as described by Kaler (1976) in order to derive absolute fluxes; 55 Cyg was used as a standard. The relative continuum flux-densities for He 2-467 are presented in Table III, and are compared with those derived from LL's Figures 2 and 3.…”

Section: Resultsmentioning

confidence: 99%

“…Lutz (1977) showed that the KÀ4686) He ii/î(HAE) ratio had approximately tripled between July 1974 and July 1975. Also, the spectrum of He 2-467 is similar to that of AG Draconis (Lutz 1977), which is well known to be variable (e.g., Boyarchuk 1968;Lutz, Lutz, and Kaler 1977). Boyarchuk (1968) and Swings and Allen (1972) also refer to AG Dra as a symbiotic star, consistent with our reference to He 2-467 as a YSS.…”

Section: Introduction II Observationsmentioning

confidence: 99%

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He 2-467 - A yellow symbiotic star

Kaler¹,

Lutz²

1980

PASP

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“…The variation between these two dates for F(A4686)/H/? is similar to the variation initially detected by Lutz (1977).…”

Section: Resultssupporting

confidence: 88%

Section: Resultsmentioning

confidence: 99%

Section: Introduction II Observationsmentioning

confidence: 99%

See 1 more Smart Citation

He 2-467 - A yellow symbiotic star

Kaler¹,

Lutz²

1980

PASP

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“…Obreschkow et al (2016) proposed a hybrid stability model that predicts the mass fraction of atomic (hydrogen+helium) gas as a function of mass and specific angular momentum of the whole (gas+stars) disc, assuming a constant H i velocity dispersion: fHI = min{1, 2.5 q 1.12 }, where q = j disc σHI/GM disc and σHI = 10 km s −1 . Such a ⋆ E-mail: romeo@chalmers.se stability model has been tested in a variety of applications (e.g., Lagos et al 2017;Lutz et al 2017Lutz et al , 2018Stevens et al 2018;Wang et al 2018;Džudžar et al 2019;Murugeshan et al 2019;Stevens et al 2019). Another important contribution is the one by Zasov & Zaitseva (2017), who showed that the relation between atomic gas mass and disc specific angular momentum is equally well described by a simpler stability model controlled by Qgas, the gas Toomre parameter, assuming that Qgas is approximately constant within a galaxy (like σgas).…”

Section: Introductionmentioning

confidence: 99%

From massive spirals to dwarf irregulars: a new set of tight scaling relations for cold gas and stars driven by disc gravitational instability

Romeo

2019

Monthly Notices of the Royal Astronomical Society

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We present a new galaxy scaling relation that predicts the mass fractions of atomic gas, molecular gas and stars as a function of fundamental physical properties such as mass and specific angular momentum. Our scaling relation stretches across two orders of magnitude in mass fraction, and applies to galaxies of any morphological type from Sa to dIrr, thus spanning five orders of magnitude in stellar mass. It has a 1σ scatter of 0.2 dex, a correlation coefficient of 0.8 and a significance level close to 0, which means that the correlation between measured and predicted mass fractions is tight, strong and significant. The new scaling relation is not a best-fitting relation and has no free parameters, but originates from the low galaxy-to-galaxy variance of Q , the mass-weighted average of Toomre's Q stability parameter. This is in contrast to the variance/variation of Q within a galaxy, which is particularly large for atomic gas.

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“…The cool component of the system LT Del has been classified repeatedly. Initially, Lutz et al (1976) assigned the spectral type G to the star based on the presence of the G band and the CaI λ4226 absorption line in the spectrum. Subsequently, Munari and Buson (1992) obtained an estimate of G6III from the infrared (IR) CaII triplet.…”

Section: Introductionmentioning

confidence: 99%

Spectrum of the Yellow Symbiotic Star LT Delphini before, during, and after the 2017 Outburst

et al. 2019

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LT Del is a yellow symbiotic system that consists of a bright K3-type giant and a hot subdwarf with a temperature ∼ 10 5 K. We present the results of our spectroscopic observations of LT Del over the period 2010-2018. In 2017 the star experienced a second low-amplitude (∆V ∼ 0. m 7) outburst in the history of its studies. The emission spectrum of the star represented in the optical range by hydrogen, neutral and ionized helium lines underwent significant changes in the outburst. The fluxes in the HI and HeI emission lines increased by a factor of 5-6, the HeII λ4686 line grew by a factor of 10. According to our estimates, in the 2017 outburst the temperature of the exciting star rose to T hot ∼130 000 K, while during the first 1994 outburst the change in temperature was insignificant. This suggests cool and hot outbursts of LT Del by analogy with similar events of another yellow symbiotic star, AG Dra.

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The peculiar object He 2-467.

Cited by 14 publications

References 0 publications

He 2-467 - A yellow symbiotic star

He 2-467 - A yellow symbiotic star

From massive spirals to dwarf irregulars: a new set of tight scaling relations for cold gas and stars driven by disc gravitational instability

Spectrum of the Yellow Symbiotic Star LT Delphini before, during, and after the 2017 Outburst

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