Dynamic Imprints of Colliding-wind Dust Formation from WR 140
Carbon-rich Wolf–Rayet (WR) binaries are a prominent source of carbonaceous dust that contribute to the dust budget of galaxies. The “textbook” example of an episodic dust-producing WR binary, WR 140 (HD 193793), provides us with an ideal laboratory for investigating the dust physics and kinematics...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/2041-8213/ad9aa9 |
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| author | Emma P. Lieb Ryan M. Lau Jennifer L. Hoffman Michael F. Corcoran Macarena Garcia Marin Theodore R. Gull Kenji Hamaguchi Yinuo Han Matthew J. Hankins Olivia C. Jones Thomas I. Madura Sergey V. Marchenko Hideo Matsuhara Florentin Millour Anthony F. J. Moffat Mark R. Morris Patrick W. Morris Takashi Onaka Marshall D. Perrin Armin Rest Noel Richardson Christopher M. P. Russell Joel Sanchez-Bermudez Anthony Soulain Peter Tuthill Gerd Weigelt Peredur M. Williams |
| author_facet | Emma P. Lieb Ryan M. Lau Jennifer L. Hoffman Michael F. Corcoran Macarena Garcia Marin Theodore R. Gull Kenji Hamaguchi Yinuo Han Matthew J. Hankins Olivia C. Jones Thomas I. Madura Sergey V. Marchenko Hideo Matsuhara Florentin Millour Anthony F. J. Moffat Mark R. Morris Patrick W. Morris Takashi Onaka Marshall D. Perrin Armin Rest Noel Richardson Christopher M. P. Russell Joel Sanchez-Bermudez Anthony Soulain Peter Tuthill Gerd Weigelt Peredur M. Williams |
| author_sort | Emma P. Lieb |
| collection | DOAJ |
| description | Carbon-rich Wolf–Rayet (WR) binaries are a prominent source of carbonaceous dust that contribute to the dust budget of galaxies. The “textbook” example of an episodic dust-producing WR binary, WR 140 (HD 193793), provides us with an ideal laboratory for investigating the dust physics and kinematics in an extreme environment. This study is among the first to utilize two separate JWST observations, from Cycle 1 ERS (2022 July) and Cycle 2 (2023 September), to measure WR 140’s dust kinematics and confirm its morphology. To measure the proper motions and projected velocities of the dust shells, we performed a novel point-spread function (PSF) subtraction to reduce the effects of the bright diffraction spikes and carefully aligned the Cycle 2 to the Cycle 1 images. At 7.7 μ m, through the bright feature common to 16 dust shells (C1), we find an average dust shell proper motion of 390 ± 29 mas yr ^−1 , which equates to a projected velocity of 2714 ± 188 km s ^−1 at a distance of 1.64 kpc. Our measured speeds are constant across all visible shells and consistent with previously reported dust expansion velocities. Our observations not only prove that these dusty shells are astrophysical (i.e., not associated with any PSF artifact) and originate from WR 140, but also confirm the “clumpy” morphology of the dust shells, in which identifiable substructures within certain shells persist for at least 14 months from one cycle to the next. These results support the hypothesis that clumping in the wind collision region is required for dust production in WR binaries. |
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| institution | Kabale University |
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| language | English |
| publishDate | 2025-01-01 |
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| spelling | doaj-art-995376a1c6c64ba2a26521bf9e48df5c2025-01-13T18:06:54ZengIOP PublishingThe Astrophysical Journal Letters2041-82052025-01-019791L310.3847/2041-8213/ad9aa9Dynamic Imprints of Colliding-wind Dust Formation from WR 140Emma P. Lieb0https://orcid.org/0000-0002-4660-7452Ryan M. Lau1https://orcid.org/0000-0003-0778-0321Jennifer L. Hoffman2https://orcid.org/0000-0003-1495-2275Michael F. Corcoran3Macarena Garcia Marin4https://orcid.org/0000-0003-4801-0489Theodore R. Gull5Kenji Hamaguchi6Yinuo Han7Matthew J. Hankins8Olivia C. Jones9Thomas I. Madura10Sergey V. Marchenko11Hideo Matsuhara12Florentin Millour13Anthony F. J. Moffat14Mark R. Morris15Patrick W. Morris16Takashi Onaka17https://orcid.org/0000-0002-8234-6747Marshall D. Perrin18Armin Rest19Noel Richardson20https://orcid.org/0000-0002-2806-9339Christopher M. P. Russell21https://orcid.org/0000-0002-9213-0763Joel Sanchez-Bermudez22Anthony Soulain23Peter Tuthill24Gerd Weigelt25Peredur M. Williams26https://orcid.org/0000-0002-8092-980XUniversity of Denver , Denver, CO 80210, USANOIRLab , Tucson, AZ 85719, USAUniversity of Denver , Denver, CO 80210, USACatholic University of America , Washington, DC 20064, USA; NASA Goddard Space Flight Center , Greenbelt, MD 20771, USAEuropean Space Agency , Space Telescope Science Institute, Baltimore, MD 21218, USANASA Goddard Space Flight Center , Greenbelt, MD 20771, USANASA Goddard Space Flight Center , Greenbelt, MD 20771, USA; University of Maryland Baltimore County , Catonsville, MD 21250, USACalifornia Institute of Technology , Pasadena, CA 91125, USAArkansas Tech University , Russellville, AR 72801-2222, USAUnited Kingdom Astronomy Technology Centre , Edinburgh, EH9 3HJ, UKSan Jose State University , San Jose, CA 95112, USAScience Systems and Applications , Inc., Lanham, MD 20706, USAInstitute of Space & Astronautical Science , Kanagawa, 252-5210, JapanObservatoire de la Cote d’Azur , Nice, 06300, FranceUniversite de Montreal , Montreal, Quebec, H2V 0B3, CanadaUniversity of California—Los Angeles , Los Angeles, CA 90095, USACalifornia Institute of Technology , Pasadena, CA 91125, USADepartment of Astronomy , Graduate School of Science, University of Tokyo, Tokyo 181-0015, JapanSpace Telescope Science Institute , Baltimore, MD 21218, USASpace Telescope Science Institute , Baltimore, MD 21218, USAEmbry-Riddle Aeronautical University , Prescott, AZ 86301, USADepartment of Physics and Astronomy, Bartol Research Institute, University of Delaware , Newark, DE 19716, USAInstituto de Astronomia, Universidad Nacional Autonoma de Mexico , 04510 Ciudad de México, CDMX, MexicoUniversity of Sydney , Sydney, New South Wales, NSW 2006, AustraliaUniversity of Sydney , Sydney, New South Wales, NSW 2006, AustraliaMax Planck Institute for Radio Astronomy , Bonn, D-53121, GermanyInstitute for Astronomy, University of Edinburgh , Royal Observatory, Edinburgh, EH9 3HJ, UKCarbon-rich Wolf–Rayet (WR) binaries are a prominent source of carbonaceous dust that contribute to the dust budget of galaxies. The “textbook” example of an episodic dust-producing WR binary, WR 140 (HD 193793), provides us with an ideal laboratory for investigating the dust physics and kinematics in an extreme environment. This study is among the first to utilize two separate JWST observations, from Cycle 1 ERS (2022 July) and Cycle 2 (2023 September), to measure WR 140’s dust kinematics and confirm its morphology. To measure the proper motions and projected velocities of the dust shells, we performed a novel point-spread function (PSF) subtraction to reduce the effects of the bright diffraction spikes and carefully aligned the Cycle 2 to the Cycle 1 images. At 7.7 μ m, through the bright feature common to 16 dust shells (C1), we find an average dust shell proper motion of 390 ± 29 mas yr ^−1 , which equates to a projected velocity of 2714 ± 188 km s ^−1 at a distance of 1.64 kpc. Our measured speeds are constant across all visible shells and consistent with previously reported dust expansion velocities. Our observations not only prove that these dusty shells are astrophysical (i.e., not associated with any PSF artifact) and originate from WR 140, but also confirm the “clumpy” morphology of the dust shells, in which identifiable substructures within certain shells persist for at least 14 months from one cycle to the next. These results support the hypothesis that clumping in the wind collision region is required for dust production in WR binaries.https://doi.org/10.3847/2041-8213/ad9aa9Wolf-Rayet starsBinary starsDust formation |
| spellingShingle | Emma P. Lieb Ryan M. Lau Jennifer L. Hoffman Michael F. Corcoran Macarena Garcia Marin Theodore R. Gull Kenji Hamaguchi Yinuo Han Matthew J. Hankins Olivia C. Jones Thomas I. Madura Sergey V. Marchenko Hideo Matsuhara Florentin Millour Anthony F. J. Moffat Mark R. Morris Patrick W. Morris Takashi Onaka Marshall D. Perrin Armin Rest Noel Richardson Christopher M. P. Russell Joel Sanchez-Bermudez Anthony Soulain Peter Tuthill Gerd Weigelt Peredur M. Williams Dynamic Imprints of Colliding-wind Dust Formation from WR 140 The Astrophysical Journal Letters Wolf-Rayet stars Binary stars Dust formation |
| title | Dynamic Imprints of Colliding-wind Dust Formation from WR 140 |
| title_full | Dynamic Imprints of Colliding-wind Dust Formation from WR 140 |
| title_fullStr | Dynamic Imprints of Colliding-wind Dust Formation from WR 140 |
| title_full_unstemmed | Dynamic Imprints of Colliding-wind Dust Formation from WR 140 |
| title_short | Dynamic Imprints of Colliding-wind Dust Formation from WR 140 |
| title_sort | dynamic imprints of colliding wind dust formation from wr 140 |
| topic | Wolf-Rayet stars Binary stars Dust formation |
| url | https://doi.org/10.3847/2041-8213/ad9aa9 |
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