IRAS 17449+2320: A Possible Binary System with the B[e] Phenomenon and a Strong Magnetic Field
We report the recent results of a long-term spectroscopic and photometric monitoring of IRAS 17449+2320, a member of the least studied group of objects with the B[e] phenomenon called FS CMa-type objects. The main hypothesis for explaining the strong emission-line spectra and infrared excesses of th...
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2025-03-01
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| author | Sergey Zharikov Anatoly Miroshnichenko Inna Reva Raushan Kokumbaeva Chingis Omarov Steve Danford Alicia Aarnio Nadine Manset Ashish Raj S. Drew Chojnowski Joseph Daglen |
| author_facet | Sergey Zharikov Anatoly Miroshnichenko Inna Reva Raushan Kokumbaeva Chingis Omarov Steve Danford Alicia Aarnio Nadine Manset Ashish Raj S. Drew Chojnowski Joseph Daglen |
| author_sort | Sergey Zharikov |
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| description | We report the recent results of a long-term spectroscopic and photometric monitoring of IRAS 17449+2320, a member of the least studied group of objects with the B[e] phenomenon called FS CMa-type objects. The main hypothesis for explaining the strong emission-line spectra and infrared excesses of these objects assumes an ongoing or past mass transfer between the components in binary systems. The object is the only star with a gaseous and dusty envelope, where a strong and variable magnetic field (5.5–7.2 kG) was found through the splitting of some spectral lines. Additionally, we discovered the regular appearance of a red-shifted absorption component in spectral lines of neutral hydrogen, helium, and oxygen as well as one of ionized silicon with a period of 36.13 ± 0.20 days. We show that the magnetic field strength also followed this period. The process was accompanied by increasing emission component strengths for the hydrogen lines as well as the helium and metallic absorption lines. We refined the fundamental parameters of the optical counterpart of IRAS 17449+2320 (<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><msub><mi mathvariant="normal">T</mi><mi>eff</mi></msub><mo>=</mo><mn>9800</mn><mo>±</mo><mn>300</mn></mrow></semantics></math></inline-formula> K, log L/<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><msub><mi mathvariant="normal">L</mi><mo>⊙</mo></msub><mo>=</mo><mn>1.86</mn><mo>±</mo><mn>0.06</mn></mrow></semantics></math></inline-formula>, <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>v</mi><mo form="prefix">sin</mo><mi>i</mi><mo>=</mo><mn>9</mn><mo>±</mo><mn>2</mn></mrow></semantics></math></inline-formula> km s<sup>−1</sup>) and concluded that the star was slightly metal-deficient and viewed nearly pole-on. No signs of a secondary component were found. Possible interpretations of the observed phenomena are suggested, and some earlier findings about the object’s nature are revised. |
| format | Article |
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| institution | DOAJ |
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| spelling | doaj-art-032a68acf7ca4591b36b659e0a08cd832025-08-20T03:13:47ZengMDPI AGGalaxies2075-44342025-03-011323210.3390/galaxies13020032IRAS 17449+2320: A Possible Binary System with the B[e] Phenomenon and a Strong Magnetic FieldSergey Zharikov0Anatoly Miroshnichenko1Inna Reva2Raushan Kokumbaeva3Chingis Omarov4Steve Danford5Alicia Aarnio6Nadine Manset7Ashish Raj8S. Drew Chojnowski9Joseph Daglen10Instituto de Astronomía, Universidad Nacional Autónoma de México, AP 106, Ensenada 22800, BC, MexicoDepartment of Physics and Astronomy, University of North Carolina, Greensboro, NC 27402, USAFesenkov Astrophysical Institute, Observatory 23, Almaty 050023, KazakhstanFesenkov Astrophysical Institute, Observatory 23, Almaty 050023, KazakhstanFesenkov Astrophysical Institute, Observatory 23, Almaty 050023, KazakhstanDepartment of Physics and Astronomy, University of North Carolina, Greensboro, NC 27402, USADepartment of Physics and Astronomy, University of North Carolina, Greensboro, NC 27402, USACanada-France-Hawaii Telescope Corporation, 65-1238 Mamalahoa Hwy, Kamuela, HI 96743, USAIndian Centre for Space Physics, 466 Barakhola, Netai Nagar, Kolkata 700099, West Bengal, IndiaNASA Ames Research Center, Moffett Field, CA 94035, USADaglen Observatory, Mayhill, NM 88339, USAWe report the recent results of a long-term spectroscopic and photometric monitoring of IRAS 17449+2320, a member of the least studied group of objects with the B[e] phenomenon called FS CMa-type objects. The main hypothesis for explaining the strong emission-line spectra and infrared excesses of these objects assumes an ongoing or past mass transfer between the components in binary systems. The object is the only star with a gaseous and dusty envelope, where a strong and variable magnetic field (5.5–7.2 kG) was found through the splitting of some spectral lines. Additionally, we discovered the regular appearance of a red-shifted absorption component in spectral lines of neutral hydrogen, helium, and oxygen as well as one of ionized silicon with a period of 36.13 ± 0.20 days. We show that the magnetic field strength also followed this period. The process was accompanied by increasing emission component strengths for the hydrogen lines as well as the helium and metallic absorption lines. We refined the fundamental parameters of the optical counterpart of IRAS 17449+2320 (<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><msub><mi mathvariant="normal">T</mi><mi>eff</mi></msub><mo>=</mo><mn>9800</mn><mo>±</mo><mn>300</mn></mrow></semantics></math></inline-formula> K, log L/<inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><msub><mi mathvariant="normal">L</mi><mo>⊙</mo></msub><mo>=</mo><mn>1.86</mn><mo>±</mo><mn>0.06</mn></mrow></semantics></math></inline-formula>, <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>v</mi><mo form="prefix">sin</mo><mi>i</mi><mo>=</mo><mn>9</mn><mo>±</mo><mn>2</mn></mrow></semantics></math></inline-formula> km s<sup>−1</sup>) and concluded that the star was slightly metal-deficient and viewed nearly pole-on. No signs of a secondary component were found. Possible interpretations of the observed phenomena are suggested, and some earlier findings about the object’s nature are revised.https://www.mdpi.com/2075-4434/13/2/32early-type starsemission line starsmagnetic fieldsspectroscopyphotometry |
| spellingShingle | Sergey Zharikov Anatoly Miroshnichenko Inna Reva Raushan Kokumbaeva Chingis Omarov Steve Danford Alicia Aarnio Nadine Manset Ashish Raj S. Drew Chojnowski Joseph Daglen IRAS 17449+2320: A Possible Binary System with the B[e] Phenomenon and a Strong Magnetic Field Galaxies early-type stars emission line stars magnetic fields spectroscopy photometry |
| title | IRAS 17449+2320: A Possible Binary System with the B[e] Phenomenon and a Strong Magnetic Field |
| title_full | IRAS 17449+2320: A Possible Binary System with the B[e] Phenomenon and a Strong Magnetic Field |
| title_fullStr | IRAS 17449+2320: A Possible Binary System with the B[e] Phenomenon and a Strong Magnetic Field |
| title_full_unstemmed | IRAS 17449+2320: A Possible Binary System with the B[e] Phenomenon and a Strong Magnetic Field |
| title_short | IRAS 17449+2320: A Possible Binary System with the B[e] Phenomenon and a Strong Magnetic Field |
| title_sort | iras 17449 2320 a possible binary system with the b e phenomenon and a strong magnetic field |
| topic | early-type stars emission line stars magnetic fields spectroscopy photometry |
| url | https://www.mdpi.com/2075-4434/13/2/32 |
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