Detection of non‐radial pulsation and faint companion in the symbiotic star CH Cyg
Identifieur interne : 000094 ( Istex/Curation ); précédent : 000093; suivant : 000095Detection of non‐radial pulsation and faint companion in the symbiotic star CH Cyg
Auteurs : E. Pedretti [Royaume-Uni] ; J. D. Monnier [États-Unis] ; S. Lacour [France] ; W. A. Traub [États-Unis] ; W. C. Danchi [États-Unis] ; P. G. Tuthill [Australie] ; N. D. Thureau ; R. Millan-Gabet [États-Unis] ; J. Berger [France] ; M. G. Lacasse [États-Unis] ; P. A. Schuller [France] ; F. P. Schloerb [États-Unis] ; N. P. Carleton [États-Unis]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2009-07-21.
English descriptors
- KwdEn :
- Acta astron, Angular diameter, Angular size, Aperture mask, April, Astrometric orbit, Astrometric positions, Astron, Astronomy department, Asymmetric, Asymmetric brightness distribution, Asymmetric line, Asymmetry, Binary, California institute, Cent change, Centre column, Circular orbit, Circular orbit solution, Closure, Closure phase, Closure phases, Coast interferometer, Convective stars, Data points, Data sets, Different epochs, Dramatic change, Dust emission, Dust shell, Dwarf companion, Ellipse, Elliptical, Elliptical model, Elliptical orbit, Emission size, Error bars, Error ellipses, Faint companion, Fekel, Flux ratio, Full width, Giant companion, Giant star, Hinkle, Infrared interferometry, Interferometry, Ionic combiner, Ionic project, Iota, Iota interferometer, Journal compilation, Keck telescope, Kraus, Large number, Likely explanation, Line ellipses, Lled circles, Major axis, Mnras, Monnier, Oifits format, Open diamonds, Orbit, Orbital, Orbital parameters, Orbital positions, Pedretti, Personal communication, Photometric, Photometric variation, Photometric variations, Physical cause, Physical mechanism, Point source, Position angle, Possible orbit, Primary star, Proc, Pulsation, Radial, Radial pulsation, Radial velocities, Radial velocity, Radial velocity curve, Radial velocity curves, Radial velocity data, Radial velocity variations, Roche lobe, Secondary period, Semimajor axis, Semiregular variables, Short period, Simple model, Skopal, Spectral type, Spie, Superposed points, Symbiotic, Symbiotic pair, Symbiotic star, Symbiotic stars, Taranova, Thorough review, Tidal interaction, Triple system, White dwarf.
- Teeft :
- Acta astron, Angular diameter, Angular size, Aperture mask, April, Astrometric orbit, Astrometric positions, Astron, Astronomy department, Asymmetric, Asymmetric brightness distribution, Asymmetric line, Asymmetry, Binary, California institute, Cent change, Centre column, Circular orbit, Circular orbit solution, Closure, Closure phase, Closure phases, Coast interferometer, Convective stars, Data points, Data sets, Different epochs, Dramatic change, Dust emission, Dust shell, Dwarf companion, Ellipse, Elliptical, Elliptical model, Elliptical orbit, Emission size, Error bars, Error ellipses, Faint companion, Fekel, Flux ratio, Full width, Giant companion, Giant star, Hinkle, Infrared interferometry, Interferometry, Ionic combiner, Ionic project, Iota, Iota interferometer, Journal compilation, Keck telescope, Kraus, Large number, Likely explanation, Line ellipses, Lled circles, Major axis, Mnras, Monnier, Oifits format, Open diamonds, Orbit, Orbital, Orbital parameters, Orbital positions, Pedretti, Personal communication, Photometric, Photometric variation, Photometric variations, Physical cause, Physical mechanism, Point source, Position angle, Possible orbit, Primary star, Proc, Pulsation, Radial, Radial pulsation, Radial velocities, Radial velocity, Radial velocity curve, Radial velocity curves, Radial velocity data, Radial velocity variations, Roche lobe, Secondary period, Semimajor axis, Semiregular variables, Short period, Simple model, Skopal, Spectral type, Spie, Superposed points, Symbiotic, Symbiotic pair, Symbiotic star, Symbiotic stars, Taranova, Thorough review, Tidal interaction, Triple system, White dwarf.
Abstract
We have detected asymmetry in the symbiotic star CH Cyg through the measurement of precision closure phase with the Integrated Optics Near‐Infrared Camera (IONIC) beam combiner, at the infrared optical telescope array interferometer. The position of the asymmetry changes with time and is correlated with the phase of the 2.1‐year period found in the radial velocity measurements for this star. We can model the time‐dependent asymmetry either as the orbit of a low‐mass companion around the M giant or as an asymmetric, 20 per cent change in brightness across the M giant. We do not detect a change in the size of the star during a 3‐year monitoring period neither with respect to time nor with respect to wavelength. We find a spherical dust shell with an emission size of 2.2 ± 0.1 D* full width at half‐maximum around the M giant star. The star to dust flux ratio is estimated to be 11.63 ± 0.3. While the most likely explanation for the 20 per cent change in brightness is non‐radial pulsation, we argue that a low‐mass companion in close orbit could be the physical cause of the pulsation. The combined effect of pulsation and low‐mass companion could explain the behaviour revealed by the radial velocity curves and the time‐dependent asymmetry detected in the closure‐phase data. If CH Cyg is a typical long secondary period variable then these variations could be explained by the effect of an orbiting low‐mass companion on the primary star.
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DOI: 10.1111/j.1365-2966.2009.14906.x
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N. D. Thureau<affiliation><mods:affiliation>School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS</mods:affiliation><wicri:noCountry code="subField">9SS</wicri:noCountry></affiliation>Le document en format XML
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Pedretti</name><affiliation><mods:affiliation>School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS</mods:affiliation></affiliation><affiliation wicri:level="1"><mods:affiliation>E-mail: ep41@st‐and.ac.uk</mods:affiliation><country wicri:rule="url">Royaume-Uni</country></affiliation></author><author><name sortKey="Monnier, J D" sort="Monnier, J D" uniqKey="Monnier J" first="J. D." last="Monnier">J. D. Monnier</name><affiliation wicri:level="1"><mods:affiliation>University of Michigan, Astronomy department, 914 Dennison bldg., 500 Church street, Ann Arbor, MI 40109, USA</mods:affiliation><country xml:lang="fr">États-Unis</country><wicri:regionArea>University of Michigan, Astronomy department, 914 Dennison bldg., 500 Church street, Ann Arbor, MI 40109</wicri:regionArea></affiliation></author><author><name sortKey="Lacour, S" sort="Lacour, S" uniqKey="Lacour S" first="S." last="Lacour">S. 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Tuthill</name><affiliation wicri:level="1"><mods:affiliation>School of Physics, Sydney University, NSW 2006, Sydney, Australia</mods:affiliation><country xml:lang="fr">Australie</country><wicri:regionArea>School of Physics, Sydney University, NSW 2006, Sydney</wicri:regionArea></affiliation></author><author><name sortKey="Thureau, N D" sort="Thureau, N D" uniqKey="Thureau N" first="N. D." last="Thureau">N. D. Thureau</name><affiliation><mods:affiliation>School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS</mods:affiliation><wicri:noCountry code="subField">9SS</wicri:noCountry></affiliation></author><author><name sortKey="Millan Abet, R" sort="Millan Abet, R" uniqKey="Millan Abet R" first="R." last="Millan-Gabet">R. Millan-Gabet</name><affiliation wicri:level="1"><mods:affiliation>Michelson Science Center, California Institute of Technology, 770 S. Wilson Ave. MS 100‐22, Pasadena, CA 91125, USA</mods:affiliation><country xml:lang="fr">États-Unis</country><wicri:regionArea>Michelson Science Center, California Institute of Technology, 770 S. Wilson Ave. MS 100‐22, Pasadena, CA 91125</wicri:regionArea></affiliation></author><author><name sortKey="Berger, J" sort="Berger, J" uniqKey="Berger J" first="J." last="Berger">J. Berger</name><affiliation wicri:level="1"><mods:affiliation>Laboratoire d'Astrophysique de l'Observatoire de Grenoble (LAOG), 414 rue de la Piscine, BP 53‐X Grenoble, France</mods:affiliation><country xml:lang="fr">France</country><wicri:regionArea>Laboratoire d'Astrophysique de l'Observatoire de Grenoble (LAOG), 414 rue de la Piscine, BP 53‐X Grenoble</wicri:regionArea></affiliation></author><author><name sortKey="Lacasse, M G" sort="Lacasse, M G" uniqKey="Lacasse M" first="M. G." last="Lacasse">M. G. 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Schloerb</name><affiliation wicri:level="1"><mods:affiliation>University of Massachusetts, Astronomy Department, Amherst, MA 01003‐4610, USA</mods:affiliation><country xml:lang="fr">États-Unis</country><wicri:regionArea>University of Massachusetts, Astronomy Department, Amherst, MA 01003‐4610</wicri:regionArea></affiliation></author><author><name sortKey="Carleton, N P" sort="Carleton, N P" uniqKey="Carleton N" first="N. P." last="Carleton">N. P. Carleton</name><affiliation wicri:level="1"><mods:affiliation>Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA</mods:affiliation><country xml:lang="fr">États-Unis</country><wicri:regionArea>Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138</wicri:regionArea></affiliation></author></analytic><monogr></monogr><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><biblScope unit="vol">397</biblScope><biblScope unit="issue">1</biblScope><biblScope unit="page" from="325">325</biblScope><biblScope unit="page" to="334">334</biblScope><biblScope unit="page-count">10</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2009-07-21">2009-07-21</date></imprint><idno type="ISSN">0035-8711</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Acta astron</term><term>Angular diameter</term><term>Angular size</term><term>Aperture mask</term><term>April</term><term>Astrometric orbit</term><term>Astrometric positions</term><term>Astron</term><term>Astronomy department</term><term>Asymmetric</term><term>Asymmetric brightness distribution</term><term>Asymmetric line</term><term>Asymmetry</term><term>Binary</term><term>California institute</term><term>Cent change</term><term>Centre column</term><term>Circular orbit</term><term>Circular orbit solution</term><term>Closure</term><term>Closure phase</term><term>Closure phases</term><term>Coast interferometer</term><term>Convective stars</term><term>Data points</term><term>Data sets</term><term>Different epochs</term><term>Dramatic change</term><term>Dust emission</term><term>Dust shell</term><term>Dwarf companion</term><term>Ellipse</term><term>Elliptical</term><term>Elliptical model</term><term>Elliptical orbit</term><term>Emission size</term><term>Error bars</term><term>Error ellipses</term><term>Faint companion</term><term>Fekel</term><term>Flux ratio</term><term>Full width</term><term>Giant companion</term><term>Giant star</term><term>Hinkle</term><term>Infrared interferometry</term><term>Interferometry</term><term>Ionic combiner</term><term>Ionic project</term><term>Iota</term><term>Iota interferometer</term><term>Journal compilation</term><term>Keck telescope</term><term>Kraus</term><term>Large number</term><term>Likely explanation</term><term>Line ellipses</term><term>Lled circles</term><term>Major axis</term><term>Mnras</term><term>Monnier</term><term>Oifits format</term><term>Open diamonds</term><term>Orbit</term><term>Orbital</term><term>Orbital parameters</term><term>Orbital positions</term><term>Pedretti</term><term>Personal communication</term><term>Photometric</term><term>Photometric variation</term><term>Photometric variations</term><term>Physical cause</term><term>Physical mechanism</term><term>Point source</term><term>Position angle</term><term>Possible orbit</term><term>Primary star</term><term>Proc</term><term>Pulsation</term><term>Radial</term><term>Radial pulsation</term><term>Radial velocities</term><term>Radial velocity</term><term>Radial velocity curve</term><term>Radial velocity curves</term><term>Radial velocity data</term><term>Radial velocity variations</term><term>Roche lobe</term><term>Secondary period</term><term>Semimajor axis</term><term>Semiregular variables</term><term>Short period</term><term>Simple model</term><term>Skopal</term><term>Spectral type</term><term>Spie</term><term>Superposed points</term><term>Symbiotic</term><term>Symbiotic pair</term><term>Symbiotic star</term><term>Symbiotic stars</term><term>Taranova</term><term>Thorough review</term><term>Tidal interaction</term><term>Triple system</term><term>White dwarf</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Acta astron</term><term>Angular diameter</term><term>Angular size</term><term>Aperture mask</term><term>April</term><term>Astrometric orbit</term><term>Astrometric positions</term><term>Astron</term><term>Astronomy department</term><term>Asymmetric</term><term>Asymmetric brightness distribution</term><term>Asymmetric line</term><term>Asymmetry</term><term>Binary</term><term>California institute</term><term>Cent change</term><term>Centre column</term><term>Circular orbit</term><term>Circular orbit solution</term><term>Closure</term><term>Closure phase</term><term>Closure phases</term><term>Coast interferometer</term><term>Convective stars</term><term>Data points</term><term>Data sets</term><term>Different epochs</term><term>Dramatic change</term><term>Dust emission</term><term>Dust shell</term><term>Dwarf companion</term><term>Ellipse</term><term>Elliptical</term><term>Elliptical model</term><term>Elliptical orbit</term><term>Emission size</term><term>Error bars</term><term>Error ellipses</term><term>Faint companion</term><term>Fekel</term><term>Flux ratio</term><term>Full width</term><term>Giant companion</term><term>Giant star</term><term>Hinkle</term><term>Infrared interferometry</term><term>Interferometry</term><term>Ionic combiner</term><term>Ionic project</term><term>Iota</term><term>Iota interferometer</term><term>Journal compilation</term><term>Keck telescope</term><term>Kraus</term><term>Large number</term><term>Likely explanation</term><term>Line ellipses</term><term>Lled circles</term><term>Major axis</term><term>Mnras</term><term>Monnier</term><term>Oifits format</term><term>Open diamonds</term><term>Orbit</term><term>Orbital</term><term>Orbital parameters</term><term>Orbital positions</term><term>Pedretti</term><term>Personal communication</term><term>Photometric</term><term>Photometric variation</term><term>Photometric variations</term><term>Physical cause</term><term>Physical mechanism</term><term>Point source</term><term>Position angle</term><term>Possible orbit</term><term>Primary star</term><term>Proc</term><term>Pulsation</term><term>Radial</term><term>Radial pulsation</term><term>Radial velocities</term><term>Radial velocity</term><term>Radial velocity curve</term><term>Radial velocity curves</term><term>Radial velocity data</term><term>Radial velocity variations</term><term>Roche lobe</term><term>Secondary period</term><term>Semimajor axis</term><term>Semiregular variables</term><term>Short period</term><term>Simple model</term><term>Skopal</term><term>Spectral type</term><term>Spie</term><term>Superposed points</term><term>Symbiotic</term><term>Symbiotic pair</term><term>Symbiotic star</term><term>Symbiotic stars</term><term>Taranova</term><term>Thorough review</term><term>Tidal interaction</term><term>Triple system</term><term>White dwarf</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We have detected asymmetry in the symbiotic star CH Cyg through the measurement of precision closure phase with the Integrated Optics Near‐Infrared Camera (IONIC) beam combiner, at the infrared optical telescope array interferometer. The position of the asymmetry changes with time and is correlated with the phase of the 2.1‐year period found in the radial velocity measurements for this star. We can model the time‐dependent asymmetry either as the orbit of a low‐mass companion around the M giant or as an asymmetric, 20 per cent change in brightness across the M giant. We do not detect a change in the size of the star during a 3‐year monitoring period neither with respect to time nor with respect to wavelength. We find a spherical dust shell with an emission size of 2.2 ± 0.1 D* full width at half‐maximum around the M giant star. The star to dust flux ratio is estimated to be 11.63 ± 0.3. While the most likely explanation for the 20 per cent change in brightness is non‐radial pulsation, we argue that a low‐mass companion in close orbit could be the physical cause of the pulsation. The combined effect of pulsation and low‐mass companion could explain the behaviour revealed by the radial velocity curves and the time‐dependent asymmetry detected in the closure‐phase data. If CH Cyg is a typical long secondary period variable then these variations could be explained by the effect of an orbiting low‐mass companion on the primary star.</div></front></TEI></record>Pour manipuler ce document sous Unix (Dilib)
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