The PULSATION OF Χ CYGNI IMAGED BY OPTICAL INTERFEROMETRY: A NOVEL TECHNIQUE TO DERIVE DISTANCE AND MASS OF MIRA STARS

Lacour, S.; Thiébaut, Éric; Perrin, G.; Meimon, Serge; Haubois, X.; Pedretti, E.; Ridgway, S. T.; Monnier, John D.; Berger, J.‐P.; Schuller, P. A.; Woodruff, Henry C.; Poncelet, A.; Coroller, H. Le; Millan-Gabet, R.; Lacasse, M. G.; Traub, Wesley A.

doi:10.1088/0004-637x/707/1/632

Cited by 34 publications

(34 citation statements)

References 60 publications

(96 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Interferometric monitoring reveals temporal variations of measured stellar diameters, as well as a strong dependence of diameters on wavelength, indicating extended, dynamical atmospheres with complex molecular layers (e.g., Burns et al 1998;Ireland et al 2004a, b;Woodruff et al 2008;Lacour et al 2009). Recent advances in high-angular-resolution techniques have made it possible to resolve the surfaces and extended atmospheres of some nearby AGB stars (e.g., Stewart et al 2016b;Ohnaka et al 2016;Wittkowski et al 2017), showing temporal changes in atmospheric structures and dust properties (e.g., Haubois et al 2015;Khouri et al 2016a;Ohnaka et al 2017).…”

Section: Pulsation Convection and Atmospheric Levitation Due To Shomentioning

confidence: 99%

Mass loss of stars on the asymptotic giant branch

Höfner

Olofsson

2018

Astron Astrophys Rev

417

376

View full text Add to dashboard Cite

As low-and intermediate-mass stars reach the asymptotic giant branch (AGB), they have developed into intriguing and complex objects that are major players in the cosmic gas/dust cycle. At this stage, their appearance and evolution are strongly affected by a range of dynamical processes. Large-scale convective flows bring newlyformed chemical elements to the stellar surface and, together with pulsations, they trigger shock waves in the extended stellar atmosphere. There, massive outflows of gas and dust have their origin, which enrich the interstellar medium and, eventually, lead to a transformation of the cool luminous giants into white dwarfs. Dust grains forming in the upper atmospheric layers play a critical role in the wind acceleration process, by scattering and absorbing stellar photons and transferring their outward-directed momentum to the surrounding gas through collisions. Recent progress in high-angularresolution instrumentation, from the visual to the radio regime, is leading to valuable new insights into the complex dynamical atmospheres of AGB stars and their windforming regions. Observations are revealing asymmetries and inhomogeneities in the photospheric and dust-forming layers which vary on time-scales of months, as well as more long-lived large-scale structures in the circumstellar envelopes. High-angularresolution observations indicate at what distances from the stars dust condensation occurs, and they give information on the chemical composition and sizes of dust grains in the close vicinity of cool giants. These are essential constraints for building B Susanne Höfner

show abstract

Section: Pulsation Convection and Atmospheric Levitation Due To Shomentioning

confidence: 99%

Mass loss of stars on the asymptotic giant branch

Höfner

Olofsson

2018

Astron Astrophys Rev

417

376

View full text Add to dashboard Cite

show abstract

“…Lattanzio & Wood (2004) and Unno et al (1989) argue that this relation yields reliable results for the AGBs. With a different calibration, the same law is employed in interferometric observations of nearby Miras and supergiants as a means of direct measurement of their luminosity and radius (e.g., Weiner et al 2003;Perrin et al 2004;Lacour et al 2009). Therefore,…”

Section: Time Variability Of Luminosity and Radiusmentioning

confidence: 99%

THE AGE AND MASS OF THE α HERCULIS TRIPLE-STAR SYSTEM FROM A MESA GRID OF ROTATING STARS WITH 1.3 ⩽M/M_☉⩽ 8.0

Moravveji¹,

Guinan²,

Khosroshahi³

et al. 2013

200

View full text Add to dashboard Cite

α 1 Her is the second closest asymptotic giant branch (AGB) star to the Sun, and the variable luminous M5 Ib-II member of a triple-stellar system containing G8 III and A9 IV-V components. However, the mass of this important star was previously uncertain, with published values ranging from ∼2-15 M . As shown by this study, its fortuitous membership in a nearby resolved triple-star system makes it possible to determine its fundamental properties including its mass and age. We present over 20 years of VRI photometry of α 1 Her as well as Wing intermediate-band near-IR TiO and NIR continuum photometry. We introduce a new photometry-based calibration technique and extract the effective temperature and luminosity of α 1 Her, in agreement with recent interferometric measures. We find average values of T eff = 3280 ± 87 K and log(L/L ) = 3.92 ± 0.14. With the MESA code, we calculate a dense grid of evolutionary tracks for Galactic low-to intermediate-mass (1.3 to 8 M ) rotating stars from the pre-main sequence phase to the advanced AGB phase. We include atomic diffusion and rotation mechanisms to treat the effects of extra elemental mixing. Based on the observed properties of the α Herculis stars, we constrain the age of the system to lie in the range 0.41 to 1.25 Gyr. Thus, the mass of α 1 Her lies in the range 2.175 M/M 3.250. We compare our model-based age inference with recent tracks of the Geneva and STAREVOL codes, and show their agreement. In the prescribed mass range for α 1 Her, the observed 12 C/ 13 C and 16 O/ 17 O ratios are consistent (within 2σ ) with the ratios predicted by the MESA, Geneva, and STAREVOL codes.

show abstract

“…MiRA is capable of dealing with any available interferometric data (complex visibilities, squared visibilities, closure phases, etc. ), and has been successfully used to process real data (e.g., Lacour et al 2008;Lacour et al 2009;Le Bouquin et al 2009;Haubois et al 2009). When phases are missed because of the atmospheric turbulence, the MiRA algorithm can directly fit the available interferometric observables without explicitly rebuilding the missing phases.…”

Section: Image Reconstruction By Miramentioning

confidence: 99%

Milli-arcsecond images of the Herbig Ae star HD 163296

Renard

Malbet

Benisty³

et al. 2010

A&A

Self Cite

View full text Add to dashboard Cite

Context. The very close environments of young stars are the hosts of fundamental physical processes, such as planet formation, stardisk interactions, mass accretion, and ejection. The complex morphological structure of these environments has been confirmed by the now quite rich data sets obtained for a few objects by near-infrared long-baseline interferometry. Aims. We gathered numerous interferometric measurements for the young star HD 163296 with various interferometers (VLTI, IOTA, KeckI and CHARA), allowing for the first time an image independent of any a priori model to be reconstructed. Methods. Using the Multi-aperture image Reconstruction Algorithm (MiRA), we reconstruct images of HD 163296 in the H and K bands. We compare these images with reconstructed images obtained from simulated data using a physical model of the environment of HD 163296.Results. We obtain model-independent H and K-band images of the surroundings of HD 163296. The images detect several significant features that we can relate to an inclined asymmetric flared disk around HD 163296 with the strongest intensity at about 4-5 mas. Because of the incomplete spatial frequency coverage, we cannot state whether each of them individually is peculiar in any way. Conclusions. For the first time, milli-arcsecond images of the environment of a young star are produced. These images confirm that the morphology of the close environment of young stars is more complex than the simple models used in the literature so far.

show abstract

The PULSATION OF Χ CYGNI IMAGED BY OPTICAL INTERFEROMETRY: A NOVEL TECHNIQUE TO DERIVE DISTANCE AND MASS OF MIRA STARS

Cited by 34 publications

References 60 publications

Mass loss of stars on the asymptotic giant branch

Mass loss of stars on the asymptotic giant branch

THE AGE AND MASS OF THE α HERCULIS TRIPLE-STAR SYSTEM FROM A MESA GRID OF ROTATING STARS WITH 1.3 ⩽M/M_☉⩽ 8.0

Milli-arcsecond images of the Herbig Ae star HD 163296

Contact Info

Product

Resources

About

The PULSATION OF Χ CYGNI IMAGED BY OPTICAL INTERFEROMETRY: A NOVEL TECHNIQUE TO DERIVE DISTANCE AND MASS OF MIRA STARS

Cited by 34 publications

References 60 publications

Mass loss of stars on the asymptotic giant branch

Mass loss of stars on the asymptotic giant branch

THE AGE AND MASS OF THE α HERCULIS TRIPLE-STAR SYSTEM FROM A MESA GRID OF ROTATING STARS WITH 1.3 ⩽M/M☉⩽ 8.0

Milli-arcsecond images of the Herbig Ae star HD 163296

Contact Info

Product

Resources

About

THE AGE AND MASS OF THE α HERCULIS TRIPLE-STAR SYSTEM FROM A MESA GRID OF ROTATING STARS WITH 1.3 ⩽M/M_☉⩽ 8.0