Is the Adult Protein-Energy Malnutrition Syndrome the Same as that Described in the Infant?

Mauron, J.; Antener, I

doi:10.1007/978-3-0348-6540-1_16

Cited by 9 publications

(9 citation statements)

References 16 publications

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“…In the optical range, resonant lines of Na or K could be useful. Mauron & Guilain (1995) did not detect any Na I/K I emission, but similarly they looked only close to the central star (5 arcsec).…”

Section: P Ro S P E C T Smentioning

confidence: 92%

The formation of a detached shell around the carbon star Y CVn

Libert

Gérard

Bertre

2007

Monthly Notices of the Royal Astronomical Society

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Y CVn is a carbon star surrounded by a detached dust shell that has been imaged by the Infrared Space Observatory at 90 microns. With the Nancay Radio Telescope we have studied the gaseous counterpart in the 21-cm HI emission line. New data have been acquired and allow to improve the signal to noise ratio on this line. The high spectral resolution line profiles obtained at the position of the star and at several offset positions set strong constraints on the gas temperature and kinematics within the detached shell; the bulk of the material should be at ~ 100-200 K and in expansion at ~ 1-2 km/s. In addition, the line profile at the central position shows a quasi-rectangular pedestal that traces an 8 km/s outflow of ~ 1.0 10^-7 Msol/yr, stable for about 2 10^4 years, which corresponds to the central outflow already studied with CO rotational lines. We present a model in which the detached shell results from the slowing-down of the stellar wind by surrounding matter. The inner radius corresponds to the location where the stellar outflow is abruptly slowed down from ~ 8 km/s to 2 km/s (termination shock). The outer radius corresponds to the location where external matter is compressed by the expanding shell (bow shock). In this model the mass loss rate of Y CVn has been set constant, at the same level of 1.0 10^-7 Msol/yr, for ~ 4.5 10^5 years. The gas temperature varies from ~ 1800 K at the inner limit to 165 K at the interface between circumstellar matter and external matter. Our modelling shows that the presence of a detached shell around an AGB star may not mean that a drastic reduction of the mass loss rate has occurred in the past. The inner radius of such a shell might only be the effect of a termination shock rather than of an interruption of the mass loss process.Comment: Accepted for publication in Monthly Notices of the Royal Astronomical Societ

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Section: P Ro S P E C T Smentioning

confidence: 92%

The formation of a detached shell around the carbon star Y CVn

Libert

Gérard

Bertre

2007

Monthly Notices of the Royal Astronomical Society

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“…As shown in Table 5 our adopted current observed mass loss rate is 2 ± 1 × 10 −6 M ⊙ y −1 with a total ejected mass of 0.09 ± 0.05 M ⊙ (Knapp & Morris 1985;Glassgold & Huggins 1986;Bowers & Knapp 1987;Skinner & Whitmore 1988;Mauron 1990;Marshall et al 1992;Young et al 1993;Huggins et al 1994;Mauron et al 1995;Guilain & Mauron 1996;Harper et al 2001;Plez et al 2002;Ryde et al 2006;Le Bertre et al 2012;Humphreys 2013;Richards 2013).…”

Section: Mass Lossmentioning

confidence: 94%

“…−267 Wilson et al (1997) 58 ± 2 817 +260 Knapp et al (1985) 6 × 10 −7 Glassgold et al (1986) 4 × 10 −6 Bowers et al (1987) 9 × 10 −7 Skinner et al (1988) 1.5 × 10 −6 Mauron (1990) 4 × 10 −6 3 Marshall et al (1992) 2 × 10 −7 Young et al (1993) 5.7 × 10 −7 0.042 Huggins et al (1994) 2. × 10 −6 Mauron et al (1995) 2 − 4 × 10 −6 Guilain & Mauron (1996) 2 × 10 −6 Noriega-Crespo et al (1997) 0.034 ± 0.016 Ryde et al (1999) 2 × 10 −6 Harper et al (2001) 3.1 ± 1.3 × 10 −6 Plez et al (2002) 2 × 10 −6 Buscher et al (1990) 10 − 15% Wilson et al (1992) 12 ± 3% 6 Tuthill et al (1997) 11 − 23% 2 − 6% Wilson et al (1997) 13.1 − 15.0% 600 4.0 − 7.3% 6.1 − 8.5% Gilliland et al (1996) 200 Lobel et al (2001) 12 ± 1 12 Le Bertre (2012) 1.2 × 10 −6 0.086 14 Adopted 2 ± 1 × 10 −6 .09 ± 0.05 12 ± 12% 400 ± 200 9 ± 6…”

Section: −9mentioning

confidence: 99%

“…A shell of circumstellar material has also been detected around this star (Noriega-Crespo et al 1997;Lobel & Dupree 2001, and it appears to be losing mass at a rate of ∼ 1-3 ×10 −6 M ⊙ y −1 (Knapp & Morris 1985;Glassgold & Huggins 1986;Bowers & Knapp 1987;Skinner & Whitmore 1987;Mauron 1990;Marshall et al 1992;Young et al 1993;Huggins et al 1994;Mauron et al 1995;Guilain & Mauron 1996;Plez et al 2002;Ryde et al 2006;Harper et al 2001Harper et al , 2008LeBertre et al 2012;O'Gorman et al 2015;Kervella, et al 2016).…”

Section: Introductionmentioning

confidence: 97%

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Evolutionary Tracks for Betelgeuse

Dolan

Mathews

Lam

et al. 2016

ApJ

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We have constructed a series of non-rotating quasi-hydrostatic evolutionary models for the M2 Iab supergiant Betelgeuse (α Orionis). Our models are constrained by multiple observed values for the temperature, luminosity, surface composition and mass loss for this star, along with the parallax distance and high resolution imagery that determines its radius. We have then applied our best-fit models to analyze the observed variations in surface luminosity and the size of detected surface bright spots as the result of up-flowing convective material from regions of high temperature in the surface convective zone. We also attempt to explain the intermittently observed periodic variability in a simple radial linear adiabatic pulsation model. Based upon the best fit to all observed data, we suggest a best progenitor mass estimate of 20 +5 −3 M ⊙ and a current age from the start of the zero-age main sequence of 8.0 − 8.5 Myr based upon the observed ejected mass while on the giant branch.

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“…Various structures have been revealed and point towards an episodic and inhomogeneous mass loss. Clumps have been observed in the optical and infrared, for example in the K I line (Plez & Lambert 2002), Na I and K I (Mauron & Guilain 1995), and CO at 4.6 µm (Smith et al 2009). Recently, Kervella et al (2018) have hypothesized that the poles of the star may be the location of long lived giant convective cells observed by Montargès et al (2016) and O'Gorman et al (2017) that could be responsible for the dusty structure observed in visible linear polarization with VLT/SPHERE (Kervella et al 2016).…”

Section: Comparison With Other Nearby Red Supergiant Starsmentioning

confidence: 99%

NOEMA maps the CO J = 2 − 1 environment of the red supergiant $\mu$ Cep★

Montargès

Homan

Keller

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Red supergiant stars are surrounded by a gaseous and dusty circumstellar environment created by their mass loss which spreads heavy elements into the interstellar medium. The structure and the dynamics of this envelope are crucial to understand the processes driving the red supergiant mass loss and the shaping of the pre-supernova ejecta. We have observed the emission from the CO J = 2 − 1 line from the red supergiant star µ Cep with the NOEMA interferometer. In the line the synthesized beam was 0.92 × 0.72 arcsec (590 × 462 au at 641 pc). The continuum map shows only the unresolved contribution of the free-free emission of the star chromosphere. The continuum-subtracted channel maps reveal a very inhomogeneous and clumpy circumstellar environment. In particular, we detected a bright CO clump, as bright as the central source in the line, at 1.80 arcsec south-west from the star, in the blue channel maps. After a deprojection of the radial velocity assuming two different constant wind velocities, the observations were modelled using the 3D radiative transfer code lime to derive the characteristics of the different structures. We determine that the gaseous clumps observed around µ Cep are responsible for a mass loss rate of (4.9 ± 1.0) × 10 −7 M yr −1 , in addition to a spatially unresolved wind component with an estimated mass-loss rate of 2.0 × 10 −6 M yr −1 . Therefore, the clumps have a significant role in µ Cep's mass loss (≥ 25%). We cannot exclude that the unresolved central outflow may be made of smaller unresolved clumps.

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Is the Adult Protein-Energy Malnutrition Syndrome the Same as that Described in the Infant?

Cited by 9 publications

References 16 publications

The formation of a detached shell around the carbon star Y CVn

The formation of a detached shell around the carbon star Y CVn

Evolutionary Tracks for Betelgeuse

NOEMA maps the CO J = 2 − 1 environment of the red supergiant $\mu$ Cep★

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