AustralieFrV1, Istex, Corpus, bibRecord, 000094

Detection of non‐radial pulsation and faint companion in the symbiotic star CH Cyg

Identifieur interne : 000094 ( Istex/Corpus ); précédent : 000093; suivant : 000095

Detection of non‐radial pulsation and faint companion in the symbiotic star CH Cyg

Auteurs : E. Pedretti ; J. D. Monnier ; S. Lacour ; W. A. Traub ; W. C. Danchi ; P. G. Tuthill ; N. D. Thureau ; R. Millan-Gabet ; J. Berger ; M. G. Lacasse ; P. A. Schuller ; F. P. Schloerb ; N. P. Carleton

Source :

Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2009-07-21.

RBID : ISTEX:04E6E371D9665B014E04C92F71869FF8AF4FFCEA

English descriptors

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.

Url:

https://api.istex.fr/document/04E6E371D9665B014E04C92F71869FF8AF4FFCEA/fulltext/pdf

DOI: 10.1111/j.1365-2966.2009.14906.x

Links to Exploration step

ISTEX:04E6E371D9665B014E04C92F71869FF8AF4FFCEA

Le document en format XML

<record><TEI wicri:istexFullTextTei="biblStruct"><teiHeader><fileDesc><titleStmt><title xml:lang="en">Detection of non‐radial pulsation and faint companion in the symbiotic star CH Cyg</title>
<author><name sortKey="Pedretti, E" sort="Pedretti, E" uniqKey="Pedretti E" first="E." last="Pedretti">E. Pedretti</name>
<affiliation><mods:affiliation>School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS</mods:affiliation>
</affiliation>
<affiliation><mods:affiliation>E-mail: ep41@st‐and.ac.uk</mods:affiliation>
</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><mods:affiliation>University of Michigan, Astronomy department, 914 Dennison bldg., 500 Church street, Ann Arbor, MI 40109, USA</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Lacour, S" sort="Lacour, S" uniqKey="Lacour S" first="S." last="Lacour">S. Lacour</name>
<affiliation><mods:affiliation>Laboratoire d'Astrophysique de l'Observatoire de Grenoble (LAOG), 414 rue de la Piscine, BP 53‐X Grenoble, France</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Traub, W A" sort="Traub, W A" uniqKey="Traub W" first="W. A." last="Traub">W. A. Traub</name>
<affiliation><mods:affiliation>Jet Propulsion Laboratory, California Institute of Technology, M/S 301–451, 4800 Oak Grove Drive, Pasadena, CA 91109, USA</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Danchi, W C" sort="Danchi, W C" uniqKey="Danchi W" first="W. C." last="Danchi">W. C. Danchi</name>
<affiliation><mods:affiliation>NASA Goddard Space Flight Center, 8800, Greenbelt Road, Greenbelt, MD 20771, USA</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Tuthill, P G" sort="Tuthill, P G" uniqKey="Tuthill P" first="P. G." last="Tuthill">P. G. Tuthill</name>
<affiliation><mods:affiliation>School of Physics, Sydney University, NSW 2006, Sydney, Australia</mods:affiliation>
</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>
</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><mods:affiliation>Michelson Science Center, California Institute of Technology, 770 S. Wilson Ave. MS 100‐22, Pasadena, CA 91125, USA</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Berger, J" sort="Berger, J" uniqKey="Berger J" first="J." last="Berger">J. Berger</name>
<affiliation><mods:affiliation>Laboratoire d'Astrophysique de l'Observatoire de Grenoble (LAOG), 414 rue de la Piscine, BP 53‐X Grenoble, France</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Lacasse, M G" sort="Lacasse, M G" uniqKey="Lacasse M" first="M. G." last="Lacasse">M. G. Lacasse</name>
<affiliation><mods:affiliation>Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Schuller, P A" sort="Schuller, P A" uniqKey="Schuller P" first="P. A." last="Schuller">P. A. Schuller</name>
<affiliation><mods:affiliation>Institut d'Astrophysique Spatiale, Universit Paris–Sud, bâtiment 121, 91405 Orsay Cedex, France</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Schloerb, F P" sort="Schloerb, F P" uniqKey="Schloerb F" first="F. P." last="Schloerb">F. P. Schloerb</name>
<affiliation><mods:affiliation>University of Massachusetts, Astronomy Department, Amherst, MA 01003‐4610, USA</mods:affiliation>
</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><mods:affiliation>Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA</mods:affiliation>
</affiliation>
</author>
</titleStmt>
<publicationStmt><idno type="wicri:source">ISTEX</idno>
<idno type="RBID">ISTEX:04E6E371D9665B014E04C92F71869FF8AF4FFCEA</idno>
<date when="2009" year="2009">2009</date>
<idno type="doi">10.1111/j.1365-2966.2009.14906.x</idno>
<idno type="url">https://api.istex.fr/document/04E6E371D9665B014E04C92F71869FF8AF4FFCEA/fulltext/pdf</idno>
<idno type="wicri:Area/Istex/Corpus">000094</idno>
<idno type="wicri:explorRef" wicri:stream="Istex" wicri:step="Corpus" wicri:corpus="ISTEX">000094</idno>
</publicationStmt>
<sourceDesc><biblStruct><analytic><title level="a" type="main">Detection of non‐radial pulsation and faint companion in the symbiotic star CH Cyg</title>
<author><name sortKey="Pedretti, E" sort="Pedretti, E" uniqKey="Pedretti E" first="E." last="Pedretti">E. Pedretti</name>
<affiliation><mods:affiliation>School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS</mods:affiliation>
</affiliation>
<affiliation><mods:affiliation>E-mail: ep41@st‐and.ac.uk</mods:affiliation>
</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><mods:affiliation>University of Michigan, Astronomy department, 914 Dennison bldg., 500 Church street, Ann Arbor, MI 40109, USA</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Lacour, S" sort="Lacour, S" uniqKey="Lacour S" first="S." last="Lacour">S. Lacour</name>
<affiliation><mods:affiliation>Laboratoire d'Astrophysique de l'Observatoire de Grenoble (LAOG), 414 rue de la Piscine, BP 53‐X Grenoble, France</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Traub, W A" sort="Traub, W A" uniqKey="Traub W" first="W. A." last="Traub">W. A. Traub</name>
<affiliation><mods:affiliation>Jet Propulsion Laboratory, California Institute of Technology, M/S 301–451, 4800 Oak Grove Drive, Pasadena, CA 91109, USA</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Danchi, W C" sort="Danchi, W C" uniqKey="Danchi W" first="W. C." last="Danchi">W. C. Danchi</name>
<affiliation><mods:affiliation>NASA Goddard Space Flight Center, 8800, Greenbelt Road, Greenbelt, MD 20771, USA</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Tuthill, P G" sort="Tuthill, P G" uniqKey="Tuthill P" first="P. G." last="Tuthill">P. G. Tuthill</name>
<affiliation><mods:affiliation>School of Physics, Sydney University, NSW 2006, Sydney, Australia</mods:affiliation>
</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>
</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><mods:affiliation>Michelson Science Center, California Institute of Technology, 770 S. Wilson Ave. MS 100‐22, Pasadena, CA 91125, USA</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Berger, J" sort="Berger, J" uniqKey="Berger J" first="J." last="Berger">J. Berger</name>
<affiliation><mods:affiliation>Laboratoire d'Astrophysique de l'Observatoire de Grenoble (LAOG), 414 rue de la Piscine, BP 53‐X Grenoble, France</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Lacasse, M G" sort="Lacasse, M G" uniqKey="Lacasse M" first="M. G." last="Lacasse">M. G. Lacasse</name>
<affiliation><mods:affiliation>Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Schuller, P A" sort="Schuller, P A" uniqKey="Schuller P" first="P. A." last="Schuller">P. A. Schuller</name>
<affiliation><mods:affiliation>Institut d'Astrophysique Spatiale, Universit Paris–Sud, bâtiment 121, 91405 Orsay Cedex, France</mods:affiliation>
</affiliation>
</author>
<author><name sortKey="Schloerb, F P" sort="Schloerb, F P" uniqKey="Schloerb F" first="F. P." last="Schloerb">F. P. Schloerb</name>
<affiliation><mods:affiliation>University of Massachusetts, Astronomy Department, Amherst, MA 01003‐4610, USA</mods:affiliation>
</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><mods:affiliation>Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA</mods:affiliation>
</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>
<istex><corpusName>wiley</corpusName>
<keywords><teeft><json:string>monnier</json:string>
<json:string>hinkle</json:string>
<json:string>symbiotic</json:string>
<json:string>mnras</json:string>
<json:string>iota</json:string>
<json:string>interferometry</json:string>
<json:string>pedretti</json:string>
<json:string>circular orbit</json:string>
<json:string>april</json:string>
<json:string>journal compilation</json:string>
<json:string>closure phase</json:string>
<json:string>ellipse</json:string>
<json:string>photometric</json:string>
<json:string>proc</json:string>
<json:string>elliptical</json:string>
<json:string>pulsation</json:string>
<json:string>asymmetry</json:string>
<json:string>binary</json:string>
<json:string>fekel</json:string>
<json:string>spie</json:string>
<json:string>elliptical orbit</json:string>
<json:string>kraus</json:string>
<json:string>astron</json:string>
<json:string>skopal</json:string>
<json:string>taranova</json:string>
<json:string>infrared interferometry</json:string>
<json:string>radial pulsation</json:string>
<json:string>closure</json:string>
<json:string>giant star</json:string>
<json:string>symbiotic stars</json:string>
<json:string>likely explanation</json:string>
<json:string>faint companion</json:string>
<json:string>radial velocity</json:string>
<json:string>data points</json:string>
<json:string>dust emission</json:string>
<json:string>symbiotic pair</json:string>
<json:string>semimajor axis</json:string>
<json:string>symbiotic star</json:string>
<json:string>open diamonds</json:string>
<json:string>giant companion</json:string>
<json:string>lled circles</json:string>
<json:string>white dwarf</json:string>
<json:string>secondary period</json:string>
<json:string>flux ratio</json:string>
<json:string>physical mechanism</json:string>
<json:string>photometric variations</json:string>
<json:string>ionic combiner</json:string>
<json:string>astrometric positions</json:string>
<json:string>oifits format</json:string>
<json:string>orbital parameters</json:string>
<json:string>cent change</json:string>
<json:string>orbital</json:string>
<json:string>radial</json:string>
<json:string>emission size</json:string>
<json:string>aperture mask</json:string>
<json:string>full width</json:string>
<json:string>keck telescope</json:string>
<json:string>angular diameter</json:string>
<json:string>short period</json:string>
<json:string>spectral type</json:string>
<json:string>closure phases</json:string>
<json:string>astronomy department</json:string>
<json:string>point source</json:string>
<json:string>thorough review</json:string>
<json:string>california institute</json:string>
<json:string>dwarf companion</json:string>
<json:string>simple model</json:string>
<json:string>error bars</json:string>
<json:string>position angle</json:string>
<json:string>physical cause</json:string>
<json:string>radial velocity curves</json:string>
<json:string>elliptical model</json:string>
<json:string>angular size</json:string>
<json:string>dust shell</json:string>
<json:string>acta astron</json:string>
<json:string>data sets</json:string>
<json:string>radial velocity variations</json:string>
<json:string>line ellipses</json:string>
<json:string>error ellipses</json:string>
<json:string>asymmetric line</json:string>
<json:string>radial velocities</json:string>
<json:string>semiregular variables</json:string>
<json:string>triple system</json:string>
<json:string>personal communication</json:string>
<json:string>primary star</json:string>
<json:string>possible orbit</json:string>
<json:string>dramatic change</json:string>
<json:string>different epochs</json:string>
<json:string>centre column</json:string>
<json:string>iota interferometer</json:string>
<json:string>superposed points</json:string>
<json:string>tidal interaction</json:string>
<json:string>circular orbit solution</json:string>
<json:string>photometric variation</json:string>
<json:string>orbital positions</json:string>
<json:string>astrometric orbit</json:string>
<json:string>coast interferometer</json:string>
<json:string>major axis</json:string>
<json:string>radial velocity curve</json:string>
<json:string>roche lobe</json:string>
<json:string>asymmetric brightness distribution</json:string>
<json:string>convective stars</json:string>
<json:string>radial velocity data</json:string>
<json:string>ionic project</json:string>
<json:string>large number</json:string>
<json:string>orbit</json:string>
<json:string>asymmetric</json:string>
</teeft>
</keywords>
<author><json:item><name>E. Pedretti</name>
<affiliations><json:string>School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS</json:string>
<json:string>E-mail: ep41@st‐and.ac.uk</json:string>
</affiliations>
</json:item>
<json:item><name>J. D. Monnier</name>
<affiliations><json:string>University of Michigan, Astronomy department, 914 Dennison bldg., 500 Church street, Ann Arbor, MI 40109, USA</json:string>
</affiliations>
</json:item>
<json:item><name>S. Lacour</name>
<affiliations><json:string>Laboratoire d'Astrophysique de l'Observatoire de Grenoble (LAOG), 414 rue de la Piscine, BP 53‐X Grenoble, France</json:string>
</affiliations>
</json:item>
<json:item><name>W. A. Traub</name>
<affiliations><json:string>Jet Propulsion Laboratory, California Institute of Technology, M/S 301–451, 4800 Oak Grove Drive, Pasadena, CA 91109, USA</json:string>
</affiliations>
</json:item>
<json:item><name>W. C. Danchi</name>
<affiliations><json:string>NASA Goddard Space Flight Center, 8800, Greenbelt Road, Greenbelt, MD 20771, USA</json:string>
</affiliations>
</json:item>
<json:item><name>P. G. Tuthill</name>
<affiliations><json:string>School of Physics, Sydney University, NSW 2006, Sydney, Australia</json:string>
</affiliations>
</json:item>
<json:item><name>N. D. Thureau</name>
<affiliations><json:string>School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS</json:string>
</affiliations>
</json:item>
<json:item><name>R. Millan‐Gabet</name>
<affiliations><json:string>Michelson Science Center, California Institute of Technology, 770 S. Wilson Ave. MS 100‐22, Pasadena, CA 91125, USA</json:string>
</affiliations>
</json:item>
<json:item><name>J.‐P. Berger</name>
<affiliations><json:string>Laboratoire d'Astrophysique de l'Observatoire de Grenoble (LAOG), 414 rue de la Piscine, BP 53‐X Grenoble, France</json:string>
</affiliations>
</json:item>
<json:item><name>M. G. Lacasse</name>
<affiliations><json:string>Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA</json:string>
</affiliations>
</json:item>
<json:item><name>P. A. Schuller</name>
<affiliations><json:string>Institut d'Astrophysique Spatiale, Universit Paris–Sud, bâtiment 121, 91405 Orsay Cedex, France</json:string>
</affiliations>
</json:item>
<json:item><name>F. P. Schloerb</name>
<affiliations><json:string>University of Massachusetts, Astronomy Department, Amherst, MA 01003‐4610, USA</json:string>
</affiliations>
</json:item>
<json:item><name>N. P. Carleton</name>
<affiliations><json:string>Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA</json:string>
</affiliations>
</json:item>
</author>
<subject><json:item><lang><json:string>eng</json:string>
</lang>
<value>techniques: high angular resolution</value>
</json:item>
<json:item><lang><json:string>eng</json:string>
</lang>
<value>techniques: interferometric</value>
</json:item>
<json:item><lang><json:string>eng</json:string>
</lang>
<value>binaries: symbiotic</value>
</json:item>
<json:item><lang><json:string>eng</json:string>
</lang>
<value>stars: imaging</value>
</json:item>
<json:item><lang><json:string>eng</json:string>
</lang>
<value>stars: individual: CH Cygni</value>
</json:item>
</subject>
<articleId><json:string>MNR14906</json:string>
</articleId>
<arkIstex>ark:/67375/WNG-ZMZHK3RV-B</arkIstex>
<language><json:string>eng</json:string>
</language>
<originalGenre><json:string>article</json:string>
</originalGenre>
<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.</abstract>
<qualityIndicators><score>9.928</score>
<pdfWordCount>6937</pdfWordCount>
<pdfCharCount>37911</pdfCharCount>
<pdfVersion>1.4</pdfVersion>
<pdfPageCount>10</pdfPageCount>
<pdfPageSize>595.274 x 782.286 pts</pdfPageSize>
<refBibsNative>true</refBibsNative>
<abstractWordCount>244</abstractWordCount>
<abstractCharCount>1451</abstractCharCount>
<keywordCount>5</keywordCount>
</qualityIndicators>
<title>Detection of non‐radial pulsation and faint companion in the symbiotic star CH Cyg</title>
<genre><json:string>article</json:string>
</genre>
<host><title>Monthly Notices of the Royal Astronomical Society</title>
<language><json:string>unknown</json:string>
</language>
<doi><json:string>10.1111/(ISSN)1365-2966</json:string>
</doi>
<issn><json:string>0035-8711</json:string>
</issn>
<eissn><json:string>1365-2966</json:string>
</eissn>
<publisherId><json:string>MNR</json:string>
</publisherId>
<volume>397</volume>
<issue>1</issue>
<pages><first>325</first>
<last>334</last>
<total>10</total>
</pages>
<genre><json:string>journal</json:string>
</genre>
</host>
<namedEntities><unitex><date><json:string>2009</json:string>
<json:string>2005</json:string>
<json:string>2001</json:string>
<json:string>3200</json:string>
<json:string>2006</json:string>
<json:string>2004 to 2006</json:string>
<json:string>1999</json:string>
<json:string>1984</json:string>
<json:string>2004</json:string>
</date>
<geogName></geogName>
<orgName><json:string>Astronomy Department, Amherst, MA</json:string>
<json:string>University of Massachusetts</json:string>
<json:string>California Institute of Technology</json:string>
<json:string>Michelson Science Center</json:string>
<json:string>Jet Propulsion Laboratory, California Institute of Technology</json:string>
<json:string>Sydney University</json:string>
<json:string>Harvard–Smithsonian Center for Astrophysics</json:string>
</orgName>
<orgName_funder></orgName_funder>
<orgName_provider></orgName_provider>
<persName><json:string>C. Danchi</json:string>
<json:string>P. A. Schuller</json:string>
<json:string>N. Thureau</json:string>
<json:string>Francis Fekel</json:string>
<json:string>John Monnier</json:string>
<json:string>G. Lacasse</json:string>
<json:string>Kenneth Hinkle</json:string>
<json:string>S. Lacour</json:string>
<json:string>P. G. Tuthill</json:string>
<json:string>Leslie Hebb</json:string>
<json:string>Craig Marquardt</json:string>
<json:string>The</json:string>
<json:string>J. D. Monnier</json:string>
<json:string>Wilson Ave</json:string>
<json:string>E. Pedretti</json:string>
<json:string>D. Thureau</json:string>
<json:string>John Young</json:string>
<json:string>P. Berger</json:string>
<json:string>F. P. Schloerb</json:string>
<json:string>A. Traub</json:string>
<json:string>Cyg</json:string>
</persName>
<placeName><json:string>Ann Arbor</json:string>
<json:string>Australia</json:string>
<json:string>Grenoble</json:string>
<json:string>Strasbourg</json:string>
<json:string>CA</json:string>
<json:string>MA</json:string>
<json:string>MI</json:string>
<json:string>France</json:string>
<json:string>Cambridge</json:string>
<json:string>Pasadena</json:string>
<json:string>Sydney</json:string>
</placeName>
<ref_url><json:string>http://www.astro.lsa.umich.edu/monnier/oi_data/index.html</json:string>
<json:string>http://www.mrao.cam.ac.uk/research/OAS/oi_data/oi</json:string>
<json:string>http://cow.physics.wisc.edu/craigm/idl/</json:string>
</ref_url>
<ref_bibl><json:string>Mennesson et al. 2002</json:string>
<json:string>NASA Goddard Space Flight Center, 8800</json:string>
<json:string>Monnier et al. 2004</json:string>
<json:string>E. Pedretti et al.</json:string>
<json:string>Kraus et al. 2005</json:string>
<json:string>Hinkle et al. 1993</json:string>
<json:string>Hinkle et al. 2006</json:string>
<json:string>Berger et al. 2001</json:string>
<json:string>Wood et al. (1999)</json:string>
<json:string>Skopal et al. 1996</json:string>
<json:string>Sokoloski & Kenyon 2003</json:string>
<json:string>Kawaler (2004)</json:string>
<json:string>Ragland et al. 2008</json:string>
<json:string>Skopal et al. (1996)</json:string>
<json:string>Monnier et al. 2003</json:string>
<json:string>Balega et al. (2007)</json:string>
<json:string>Millan-Gabet et al. 2006</json:string>
<json:string>Hughes & Wood 1990</json:string>
<json:string>Zhao et al. 2007</json:string>
<json:string>Eyres et al. 2002</json:string>
<json:string>Ohnaka et al. 2003</json:string>
<json:string>Biller et al. (2006)</json:string>
<json:string>Absil et al. (2006)</json:string>
<json:string>Mikolajewski, Mikolajewska & Khudyakova 1992</json:string>
<json:string>Taranova & Iudin 1988</json:string>
<json:string>Eaton 2008</json:string>
<json:string>Tuthill et al. (2000)</json:string>
<json:string>Young et al. (2000)</json:string>
<json:string>Perrin et al. 2004</json:string>
<json:string>Joyce (2009)</json:string>
<json:string>Lacour et al. 2008</json:string>
<json:string>Hinkle et al. (2009)</json:string>
<json:string>Munari et al. 1996</json:string>
<json:string>Ragland et al. (2003)</json:string>
<json:string>Wood et al. (2004)</json:string>
<json:string>Lacour et al. (2008)</json:string>
<json:string>Iijima 1998</json:string>
<json:string>Ireland et al. 2008</json:string>
<json:string>Hale et al. (2003)</json:string>
<json:string>Mikolajewski, Mikolajewska & Tomov 1987</json:string>
<json:string>Skopal et al. 2007</json:string>
<json:string>Kraus et al. 2008</json:string>
<json:string>Hinkle et al. 2009</json:string>
<json:string>Baldwin et al. (1996)</json:string>
<json:string>Pedretti et al. (2008)</json:string>
<json:string>Traub et al. 2004</json:string>
<json:string>Monnier et al. 2006</json:string>
<json:string>van Belle et al. (2001)</json:string>
<json:string>Pauls et al. 2005</json:string>
<json:string>Hofmann et al. (2003)</json:string>
<json:string>Kraus et al. 2007</json:string>
<json:string>Hinkle et al. (1993)</json:string>
<json:string>van Leeuwen 2007</json:string>
<json:string>Berger et al. 2003</json:string>
<json:string>Schmidt et al. (2006)</json:string>
<json:string>Schild et al. (1999)</json:string>
<json:string>Soszynski et al. (2007)</json:string>
<json:string>Deutsch et al. 1974</json:string>
<json:string>Hinkle et al. (2002)</json:string>
<json:string>Wood et al. 2004</json:string>
</ref_bibl>
<bibl></bibl>
</unitex>
</namedEntities>
<ark><json:string>ark:/67375/WNG-ZMZHK3RV-B</json:string>
</ark>
<categories><wos><json:string>1 - science</json:string>
<json:string>2 - astronomy & astrophysics</json:string>
</wos>
<scienceMetrix><json:string>1 - natural sciences</json:string>
<json:string>2 - physics & astronomy</json:string>
<json:string>3 - astronomy & astrophysics</json:string>
</scienceMetrix>
<scopus><json:string>1 - Physical Sciences</json:string>
<json:string>2 - Earth and Planetary Sciences</json:string>
<json:string>3 - Space and Planetary Science</json:string>
<json:string>1 - Physical Sciences</json:string>
<json:string>2 - Physics and Astronomy</json:string>
<json:string>3 - Astronomy and Astrophysics</json:string>
</scopus>
<inist><json:string>1 - sciences appliquees, technologies et medecines</json:string>
<json:string>2 - sciences biologiques et medicales</json:string>
<json:string>3 - sciences biologiques fondamentales et appliquees. psychologie</json:string>
</inist>
</categories>
<publicationDate>2009</publicationDate>
<copyrightDate>2009</copyrightDate>
<doi><json:string>10.1111/j.1365-2966.2009.14906.x</json:string>
</doi>
<id>04E6E371D9665B014E04C92F71869FF8AF4FFCEA</id>
<score>1</score>
<fulltext><json:item><extension>pdf</extension>
<original>true</original>
<mimetype>application/pdf</mimetype>
<uri>https://api.istex.fr/document/04E6E371D9665B014E04C92F71869FF8AF4FFCEA/fulltext/pdf</uri>
</json:item>
<json:item><extension>zip</extension>
<original>false</original>
<mimetype>application/zip</mimetype>
<uri>https://api.istex.fr/document/04E6E371D9665B014E04C92F71869FF8AF4FFCEA/fulltext/zip</uri>
</json:item>
<istex:fulltextTEI uri="https://api.istex.fr/document/04E6E371D9665B014E04C92F71869FF8AF4FFCEA/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main">Detection of non‐radial pulsation and faint companion in the symbiotic star CH Cyg</title>
</titleStmt>
<publicationStmt><authority>ISTEX</authority>
<publisher>Blackwell Publishing Ltd</publisher>
<pubPlace>Oxford, UK</pubPlace>
<availability><licence>© 2009 The Authors. Journal compilation © 2009 RAS</licence>
</availability>
<date type="published" when="2009-07-21"></date>
</publicationStmt>
<notesStmt><note type="content-type" subtype="article" source="article" scheme="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</note>
<note type="publication-type" subtype="journal" scheme="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</note>
</notesStmt>
<sourceDesc><biblStruct type="article"><analytic><title level="a" type="main">Detection of non‐radial pulsation and faint companion in the symbiotic star CH Cyg</title>
<title level="a" type="short">Infrared interferometry of CH Cyg</title>
<author xml:id="author-0000" role="corresp"><persName><forename type="first">E.</forename>
<surname>Pedretti</surname>
</persName>
<affiliation>School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS</affiliation>
<note type="foot">Affiliated to Scottish universities physics alliance (SUPA).</note>
<affiliation>E‐mail: ep41@st‐and.ac.uk</affiliation>
</author>
<author xml:id="author-0001"><persName><forename type="first">J. D.</forename>
<surname>Monnier</surname>
</persName>
<affiliation>University of Michigan, Astronomy department, 914 Dennison bldg., 500 Church street, Ann Arbor, MI 40109, USA<address><country key="US"></country>
</address>
</affiliation>
</author>
<author xml:id="author-0002"><persName><forename type="first">S.</forename>
<surname>Lacour</surname>
</persName>
<affiliation>Laboratoire d'Astrophysique de l'Observatoire de Grenoble (LAOG), 414 rue de la Piscine, BP 53‐X Grenoble, France<address><country key="FR"></country>
</address>
</affiliation>
</author>
<author xml:id="author-0003"><persName><forename type="first">W. A.</forename>
<surname>Traub</surname>
</persName>
<affiliation>Jet Propulsion Laboratory, California Institute of Technology, M/S 301–451, 4800 Oak Grove Drive, Pasadena, CA 91109, USA<address><country key="US"></country>
</address>
</affiliation>
</author>
<author xml:id="author-0004"><persName><forename type="first">W. C.</forename>
<surname>Danchi</surname>
</persName>
<affiliation>NASA Goddard Space Flight Center, 8800, Greenbelt Road, Greenbelt, MD 20771, USA<address><country key="US"></country>
</address>
</affiliation>
</author>
<author xml:id="author-0005"><persName><forename type="first">P. G.</forename>
<surname>Tuthill</surname>
</persName>
<affiliation>School of Physics, Sydney University, NSW 2006, Sydney, Australia<address><country key="AU"></country>
</address>
</affiliation>
</author>
<author xml:id="author-0006"><persName><forename type="first">N. D.</forename>
<surname>Thureau</surname>
</persName>
<affiliation>School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS</affiliation>
</author>
<author xml:id="author-0007"><persName><forename type="first">R.</forename>
<surname>Millan‐Gabet</surname>
</persName>
<affiliation>Michelson Science Center, California Institute of Technology, 770 S. Wilson Ave. MS 100‐22, Pasadena, CA 91125, USA<address><country key="US"></country>
</address>
</affiliation>
</author>
<author xml:id="author-0008"><persName><forename type="first">J.‐P.</forename>
<surname>Berger</surname>
</persName>
<affiliation>Laboratoire d'Astrophysique de l'Observatoire de Grenoble (LAOG), 414 rue de la Piscine, BP 53‐X Grenoble, France<address><country key="FR"></country>
</address>
</affiliation>
</author>
<author xml:id="author-0009"><persName><forename type="first">M. G.</forename>
<surname>Lacasse</surname>
</persName>
<affiliation>Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA<address><country key="US"></country>
</address>
</affiliation>
</author>
<author xml:id="author-0010"><persName><forename type="first">P. A.</forename>
<surname>Schuller</surname>
</persName>
<affiliation>Institut d'Astrophysique Spatiale, Universit Paris–Sud, bâtiment 121, 91405 Orsay Cedex, France<address><country key="FR"></country>
</address>
</affiliation>
</author>
<author xml:id="author-0011"><persName><forename type="first">F. P.</forename>
<surname>Schloerb</surname>
</persName>
<affiliation>University of Massachusetts, Astronomy Department, Amherst, MA 01003‐4610, USA<address><country key="US"></country>
</address>
</affiliation>
</author>
<author xml:id="author-0012"><persName><forename type="first">N. P.</forename>
<surname>Carleton</surname>
</persName>
<affiliation>Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA<address><country key="US"></country>
</address>
</affiliation>
</author>
<idno type="istex">04E6E371D9665B014E04C92F71869FF8AF4FFCEA</idno>
<idno type="ark">ark:/67375/WNG-ZMZHK3RV-B</idno>
<idno type="DOI">10.1111/j.1365-2966.2009.14906.x</idno>
<idno type="unit">MNR14906</idno>
<idno type="toTypesetVersion">file:MNR.MNR14906.pdf</idno>
</analytic>
<monogr><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="pISSN">0035-8711</idno>
<idno type="eISSN">1365-2966</idno>
<idno type="book-DOI">10.1111/(ISSN)1365-2966</idno>
<idno type="book-part-DOI">10.1111/mnr.2009.397.issue-1</idno>
<idno type="product">MNR</idno>
<idno type="publisherDivision">ST</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"></date>
</imprint>
</monogr>
</biblStruct>
</sourceDesc>
</fileDesc>
<profileDesc><abstract xml:lang="en" style="main"><head>ABSTRACT</head>
<p>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 <hi rend="italic">D</hi>
<hi rend="subscript">*</hi>
 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.</p>
</abstract>
<textClass><keywords xml:lang="en"><term xml:id="k1">techniques: high angular resolution</term>
<term xml:id="k2">techniques: interferometric</term>
<term xml:id="k3">binaries: symbiotic</term>
<term xml:id="k4">stars: imaging</term>
<term xml:id="k5">stars: individual: CH Cygni</term>
</keywords>
<keywords rend="tocHeading1"><term>Papers</term>
</keywords>
</textClass>
<langUsage><language ident="en"></language>
</langUsage>
</profileDesc>
</teiHeader>
</istex:fulltextTEI>
<json:item><extension>txt</extension>
<original>false</original>
<mimetype>text/plain</mimetype>
<uri>https://api.istex.fr/document/04E6E371D9665B014E04C92F71869FF8AF4FFCEA/fulltext/txt</uri>
</json:item>
</fulltext>
<metadata><istex:metadataXml wicri:clean="Wiley, elements deleted: body"><istex:xmlDeclaration>version="1.0" encoding="UTF-8" standalone="yes"</istex:xmlDeclaration>
<istex:document><component version="2.0" type="serialArticle" xml:lang="en"><header><publicationMeta level="product"><publisherInfo><publisherName>Blackwell Publishing Ltd</publisherName>
<publisherLoc>Oxford, UK</publisherLoc>
</publisherInfo>
<doi origin="wiley" registered="yes">10.1111/(ISSN)1365-2966</doi>
<issn type="print">0035-8711</issn>
<issn type="electronic">1365-2966</issn>
<idGroup><id type="product" value="MNR"></id>
<id type="publisherDivision" value="ST"></id>
</idGroup>
<titleGroup><title type="main" sort="MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY">Monthly Notices of the Royal Astronomical Society</title>
</titleGroup>
</publicationMeta>
<publicationMeta level="part" position="07001"><doi origin="wiley">10.1111/mnr.2009.397.issue-1</doi>
<numberingGroup><numbering type="journalVolume" number="397">397</numbering>
<numbering type="journalIssue" number="1">1</numbering>
</numberingGroup>
<coverDate startDate="2009-07-21">July 2009</coverDate>
</publicationMeta>
<publicationMeta level="unit" type="article" position="26" status="forIssue"><doi origin="wiley">10.1111/j.1365-2966.2009.14906.x</doi>
<idGroup><id type="unit" value="MNR14906"></id>
</idGroup>
<countGroup><count type="pageTotal" number="10"></count>
</countGroup>
<titleGroup><title type="tocHeading1">Papers</title>
</titleGroup>
<copyright>© 2009 The Authors. Journal compilation © 2009 RAS</copyright>
<eventGroup><event type="firstOnline" date="2009-06-22"></event>
<event type="publishedOnlineFinalForm" date="2009-07-10"></event>
<event type="xmlConverted" agent="Converter:BPG_TO_WML3G version:2.3.6 mode:FullText source:FullText result:FullText" date="2010-04-21"></event>
<event type="xmlConverted" agent="Converter:WILEY_ML3G_TO_WILEY_ML3GV2 version:3.8.8" date="2014-02-02"></event>
<event type="xmlConverted" agent="Converter:WML3G_To_WML3G version:4.1.7 mode:FullText,remove_FC" date="2014-11-01"></event>
</eventGroup>
<numberingGroup><numbering type="pageFirst" number="325">325</numbering>
<numbering type="pageLast" number="334">334</numbering>
</numberingGroup>
<correspondenceTo>
E‐mail: <email normalForm="ep41@st-and.ac.uk">ep41@st‐and.ac.uk</email>
</correspondenceTo>
<linkGroup><link type="toTypesetVersion" href="file:MNR.MNR14906.pdf"></link>
</linkGroup>
</publicationMeta>
<contentMeta><unparsedEditorialHistory>Accepted 2009 April 14. Received 2009 April 14; in original form 2009 February 8</unparsedEditorialHistory>
<countGroup><count type="figureTotal" number="5"></count>
<count type="tableTotal" number="7"></count>
<count type="formulaTotal" number="64"></count>
<count type="referenceTotal" number="63"></count>
<count type="linksCrossRef" number="143"></count>
</countGroup>
<titleGroup><title type="main">Detection of non‐radial pulsation and faint companion in the symbiotic star CH Cyg</title>
<title type="shortAuthors"><i>E. Pedretti et al.</i>
</title>
<title type="short"><i>Infrared interferometry of CH Cyg</i>
</title>
</titleGroup>
<creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1" noteRef="#fn4" corresponding="yes"><personName><givenNames>E.</givenNames>
<familyName>Pedretti</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr2" affiliationRef="#a2"><personName><givenNames>J. D.</givenNames>
<familyName>Monnier</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr3" affiliationRef="#a3"><personName><givenNames>S.</givenNames>
<familyName>Lacour</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr4" affiliationRef="#a4"><personName><givenNames>W. A.</givenNames>
<familyName>Traub</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr5" affiliationRef="#a5"><personName><givenNames>W. C.</givenNames>
<familyName>Danchi</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr6" affiliationRef="#a6"><personName><givenNames>P. G.</givenNames>
<familyName>Tuthill</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr7" affiliationRef="#a1"><personName><givenNames>N. D.</givenNames>
<familyName>Thureau</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr8" affiliationRef="#a7"><personName><givenNames>R.</givenNames>
<familyName>Millan‐Gabet</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr9" affiliationRef="#a3"><personName><givenNames>J.‐P.</givenNames>
<familyName>Berger</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr10" affiliationRef="#a8"><personName><givenNames>M. G.</givenNames>
<familyName>Lacasse</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr11" affiliationRef="#a9"><personName><givenNames>P. A.</givenNames>
<familyName>Schuller</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr12" affiliationRef="#a10"><personName><givenNames>F. P.</givenNames>
<familyName>Schloerb</familyName>
</personName>
</creator>
<creator creatorRole="author" xml:id="cr13" affiliationRef="#a8"><personName><givenNames>N. P.</givenNames>
<familyName>Carleton</familyName>
</personName>
</creator>
</creators>
<affiliationGroup><affiliation xml:id="a1"><unparsedAffiliation>School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS</unparsedAffiliation>
</affiliation>
<affiliation xml:id="a2" countryCode="US"><unparsedAffiliation>University of Michigan, Astronomy department, 914 Dennison bldg., 500 Church street, Ann Arbor, MI 40109, USA</unparsedAffiliation>
</affiliation>
<affiliation xml:id="a3" countryCode="FR"><unparsedAffiliation>Laboratoire d'Astrophysique de l'Observatoire de Grenoble (LAOG), 414 rue de la Piscine, BP 53‐X Grenoble, France</unparsedAffiliation>
</affiliation>
<affiliation xml:id="a4" countryCode="US"><unparsedAffiliation>Jet Propulsion Laboratory, California Institute of Technology, M/S 301–451, 4800 Oak Grove Drive, Pasadena, CA 91109, USA</unparsedAffiliation>
</affiliation>
<affiliation xml:id="a5" countryCode="US"><unparsedAffiliation>NASA Goddard Space Flight Center, 8800, Greenbelt Road, Greenbelt, MD 20771, USA</unparsedAffiliation>
</affiliation>
<affiliation xml:id="a6" countryCode="AU"><unparsedAffiliation>School of Physics, Sydney University, NSW 2006, Sydney, Australia</unparsedAffiliation>
</affiliation>
<affiliation xml:id="a7" countryCode="US"><unparsedAffiliation>Michelson Science Center, California Institute of Technology, 770 S. Wilson Ave. MS 100‐22, Pasadena, CA 91125, USA</unparsedAffiliation>
</affiliation>
<affiliation xml:id="a8" countryCode="US"><unparsedAffiliation>Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA</unparsedAffiliation>
</affiliation>
<affiliation xml:id="a9" countryCode="FR"><unparsedAffiliation>Institut d'Astrophysique Spatiale, Universit Paris–Sud, bâtiment 121, 91405 Orsay Cedex, France</unparsedAffiliation>
</affiliation>
<affiliation xml:id="a10" countryCode="US"><unparsedAffiliation>University of Massachusetts, Astronomy Department, Amherst, MA 01003‐4610, USA</unparsedAffiliation>
</affiliation>
</affiliationGroup>
<keywordGroup xml:lang="en"><keyword xml:id="k1">techniques: high angular resolution</keyword>
<keyword xml:id="k2">techniques: interferometric</keyword>
<keyword xml:id="k3">binaries: symbiotic</keyword>
<keyword xml:id="k4">stars: imaging</keyword>
<keyword xml:id="k5">stars: individual: CH Cygni</keyword>
</keywordGroup>
<abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title>
<p>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 <i>D</i>
<sub>*</sub>
 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.</p>
</abstract>
</abstractGroup>
</contentMeta>
<noteGroup><note xml:id="fn4"><label><sup>★</sup>
</label>
<p>Affiliated to Scottish universities physics alliance (SUPA).</p>
</note>
</noteGroup>
</header>
</component>
</istex:document>
</istex:metadataXml>
<mods version="3.6"><titleInfo lang="en"><title>Detection of non‐radial pulsation and faint companion in the symbiotic star CH Cyg</title>
</titleInfo>
<titleInfo type="abbreviated" lang="en"><title>Infrared interferometry of CH Cyg</title>
</titleInfo>
<titleInfo type="alternative" contentType="CDATA" lang="en"><title>Detection of non‐radial pulsation and faint companion in the symbiotic star CH Cyg</title>
</titleInfo>
<name type="personal"><namePart type="given">E.</namePart>
<namePart type="family">Pedretti</namePart>
<affiliation>School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS</affiliation>
<description>Affiliated to Scottish universities physics alliance (SUPA).</description>
<affiliation>E-mail: ep41@st‐and.ac.uk</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal"><namePart type="given">J. D.</namePart>
<namePart type="family">Monnier</namePart>
<affiliation>University of Michigan, Astronomy department, 914 Dennison bldg., 500 Church street, Ann Arbor, MI 40109, USA</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal"><namePart type="given">S.</namePart>
<namePart type="family">Lacour</namePart>
<affiliation>Laboratoire d'Astrophysique de l'Observatoire de Grenoble (LAOG), 414 rue de la Piscine, BP 53‐X Grenoble, France</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal"><namePart type="given">W. A.</namePart>
<namePart type="family">Traub</namePart>
<affiliation>Jet Propulsion Laboratory, California Institute of Technology, M/S 301–451, 4800 Oak Grove Drive, Pasadena, CA 91109, USA</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal"><namePart type="given">W. C.</namePart>
<namePart type="family">Danchi</namePart>
<affiliation>NASA Goddard Space Flight Center, 8800, Greenbelt Road, Greenbelt, MD 20771, USA</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal"><namePart type="given">P. G.</namePart>
<namePart type="family">Tuthill</namePart>
<affiliation>School of Physics, Sydney University, NSW 2006, Sydney, Australia</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal"><namePart type="given">N. D.</namePart>
<namePart type="family">Thureau</namePart>
<affiliation>School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal"><namePart type="given">R.</namePart>
<namePart type="family">Millan‐Gabet</namePart>
<affiliation>Michelson Science Center, California Institute of Technology, 770 S. Wilson Ave. MS 100‐22, Pasadena, CA 91125, USA</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal"><namePart type="given">J.‐P.</namePart>
<namePart type="family">Berger</namePart>
<affiliation>Laboratoire d'Astrophysique de l'Observatoire de Grenoble (LAOG), 414 rue de la Piscine, BP 53‐X Grenoble, France</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal"><namePart type="given">M. G.</namePart>
<namePart type="family">Lacasse</namePart>
<affiliation>Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal"><namePart type="given">P. A.</namePart>
<namePart type="family">Schuller</namePart>
<affiliation>Institut d'Astrophysique Spatiale, Universit Paris–Sud, bâtiment 121, 91405 Orsay Cedex, France</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal"><namePart type="given">F. P.</namePart>
<namePart type="family">Schloerb</namePart>
<affiliation>University of Massachusetts, Astronomy Department, Amherst, MA 01003‐4610, USA</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<name type="personal"><namePart type="given">N. P.</namePart>
<namePart type="family">Carleton</namePart>
<affiliation>Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA</affiliation>
<role><roleTerm type="text">author</roleTerm>
</role>
</name>
<typeOfResource>text</typeOfResource>
<genre type="article" displayLabel="article" authority="ISTEX" authorityURI="https://content-type.data.istex.fr" valueURI="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</genre>
<originInfo><publisher>Blackwell Publishing Ltd</publisher>
<place><placeTerm type="text">Oxford, UK</placeTerm>
</place>
<dateIssued encoding="w3cdtf">2009-07-21</dateIssued>
<edition>Accepted 2009 April 14. Received 2009 April 14; in original form 2009 February 8</edition>
<copyrightDate encoding="w3cdtf">2009</copyrightDate>
</originInfo>
<language><languageTerm type="code" authority="rfc3066">en</languageTerm>
<languageTerm type="code" authority="iso639-2b">eng</languageTerm>
</language>
<physicalDescription><extent unit="figures">5</extent>
<extent unit="tables">7</extent>
<extent unit="formulas">64</extent>
<extent unit="references">63</extent>
<extent unit="linksCrossRef">143</extent>
</physicalDescription>
<abstract 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.</abstract>
<subject lang="en"><genre>keywords</genre>
<topic>techniques: high angular resolution</topic>
<topic>techniques: interferometric</topic>
<topic>binaries: symbiotic</topic>
<topic>stars: imaging</topic>
<topic>stars: individual: CH Cygni</topic>
</subject>
<relatedItem type="host"><titleInfo><title>Monthly Notices of the Royal Astronomical Society</title>
</titleInfo>
<genre type="journal" authority="ISTEX" authorityURI="https://publication-type.data.istex.fr" valueURI="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</genre>
<identifier type="ISSN">0035-8711</identifier>
<identifier type="eISSN">1365-2966</identifier>
<identifier type="DOI">10.1111/(ISSN)1365-2966</identifier>
<identifier type="PublisherID">MNR</identifier>
<part><date>2009</date>
<detail type="volume"><caption>vol.</caption>
<number>397</number>
</detail>
<detail type="issue"><caption>no.</caption>
<number>1</number>
</detail>
<extent unit="pages"><start>325</start>
<end>334</end>
<total>10</total>
</extent>
</part>
</relatedItem>
<identifier type="istex">04E6E371D9665B014E04C92F71869FF8AF4FFCEA</identifier>
<identifier type="ark">ark:/67375/WNG-ZMZHK3RV-B</identifier>
<identifier type="DOI">10.1111/j.1365-2966.2009.14906.x</identifier>
<identifier type="ArticleID">MNR14906</identifier>
<accessCondition type="use and reproduction" contentType="copyright">© 2009 The Authors. Journal compilation © 2009 RAS</accessCondition>
<recordInfo><recordContentSource authority="ISTEX" authorityURI="https://loaded-corpus.data.istex.fr" valueURI="https://loaded-corpus.data.istex.fr/ark:/67375/XBH-L0C46X92-X">wiley</recordContentSource>
<recordOrigin>Blackwell Publishing Ltd</recordOrigin>
</recordInfo>
</mods>
<json:item><extension>json</extension>
<original>false</original>
<mimetype>application/json</mimetype>
<uri>https://api.istex.fr/document/04E6E371D9665B014E04C92F71869FF8AF4FFCEA/metadata/json</uri>
</json:item>
</metadata>
<serie></serie>
</istex>
</record>

Pour manipuler ce document sous Unix (Dilib)

EXPLOR_STEP=$WICRI_ROOT/Wicri/Asie/explor/AustralieFrV1/Data/Istex/Corpus

HfdSelect -h $EXPLOR_STEP/biblio.hfd -nk 000094 | SxmlIndent | more

HfdSelect -h $EXPLOR_AREA/Data/Istex/Corpus/biblio.hfd -nk 000094 | SxmlIndent | more

Pour mettre un lien sur cette page dans le réseau Wicri

{{Explor lien
   |wiki=    Wicri/Asie
   |area=    AustralieFrV1
   |flux=    Istex
   |étape=   Corpus
   |type=    RBID
   |clé=     ISTEX:04E6E371D9665B014E04C92F71869FF8AF4FFCEA
   |texte=   Detection of non‐radial pulsation and faint companion in the symbiotic star CH Cyg
}}

This area was generated with Dilib version V0.6.33.
Data generation: Tue Dec 5 10:43:12 2017. Site generation: Tue Mar 5 14:07:20 2024

	Serveur d'exploration sur les relations entre la France et l'Australie
	Attention, ce site est en cours de développement ! Attention, site généré par des moyens informatiques à partir de corpus bruts. Les informations ne sont donc pas validées.

Serveur d'exploration sur les relations entre la France et l'Australie

Detection of non‐radial pulsation and faint companion in the symbiotic star CH Cyg

Detection of non‐radial pulsation and faint companion in the symbiotic star CH Cyg

Source :

English descriptors

Abstract

Links to Exploration step

Le document en format XML

Pour manipuler ce document sous Unix (Dilib)

Pour mettre un lien sur cette page dans le réseau Wicri