Submillimeter-wavelength Polarimetry of IRC+10216

We present SCUBA-2/POL-2 850 μ m polarimetric observations of the circumstellar envelope (CSE) of the carbon-rich asymptotic giant branch (AGB) star IRC+10216. Both far-IR (FIR) and optical polarization data indicate grains aligned with their long axis in the radial direction relative to the central...
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Gespeichert in:

Autor*in:	B-G. Andersson [verfasserIn] Janik Karoly [verfasserIn] Pierre Bastien [verfasserIn] Archana Soam [verfasserIn] Simon Coudé [verfasserIn] Mehrnoosh Tahani [verfasserIn] Michael S. Gordon [verfasserIn] Sydney Fox-Middleton [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2024

Schlagwörter:	Circumstellar dust Magnetic fields Carbonaceous grains Asymptotic giant branch stars

Übergeordnetes Werk:	In: The Astrophysical Journal - IOP Publishing, 2022, 963(2024), 1, p 76
Übergeordnetes Werk:	volume:963 ; year:2024 ; number:1, p 76

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3847/1538-4357/ad1835

Katalog-ID:	DOAJ10165586X

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520			\|a We present SCUBA-2/POL-2 850 μ m polarimetric observations of the circumstellar envelope (CSE) of the carbon-rich asymptotic giant branch (AGB) star IRC+10216. Both far-IR (FIR) and optical polarization data indicate grains aligned with their long axis in the radial direction relative to the central star. The 850 μ m polarization does not show this simple structure. The 850 μ m data are indicative, albeit not conclusive, of a magnetic dipole geometry. Assuming such a simple dipole geometry, the resulting 850 μ m polarization geometry is consistent with both Zeeman observations and small-scale structure in the CSE. While there is significant spectral-line polarization contained within the SCUBA-2 850 μ m passband for the source, it is unlikely that our broadband polarization results are dominated by line polarization. To explain the required grain alignment, grain mineralogy effects, due to either fossil silicate grains from the earlier oxygen-rich AGB phase of the star or due to the incorporation of ferromagnetic inclusions in the largest grains, may play a role. We argue that the most likely explanation is due to a new alignment mechanism wherein a charged grain, moving relative to the magnetic field, precesses around the induced electric field and therefore aligns with the magnetic field. This mechanism is particularly attractive as the optical, FIR, and submillimeter-wave polarization of the carbon dust can then be explained in a consistent way, differing simply due to the charge state of the grains.
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allfields	10.3847/1538-4357/ad1835 doi (DE-627)DOAJ10165586X (DE-599)DOAJ6664fa8bb6be44029f141a001e2f82a5 DE-627 ger DE-627 rakwb eng QB460-466 B-G. Andersson verfasserin aut Submillimeter-wavelength Polarimetry of IRC+10216 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present SCUBA-2/POL-2 850 μ m polarimetric observations of the circumstellar envelope (CSE) of the carbon-rich asymptotic giant branch (AGB) star IRC+10216. Both far-IR (FIR) and optical polarization data indicate grains aligned with their long axis in the radial direction relative to the central star. The 850 μ m polarization does not show this simple structure. The 850 μ m data are indicative, albeit not conclusive, of a magnetic dipole geometry. Assuming such a simple dipole geometry, the resulting 850 μ m polarization geometry is consistent with both Zeeman observations and small-scale structure in the CSE. While there is significant spectral-line polarization contained within the SCUBA-2 850 μ m passband for the source, it is unlikely that our broadband polarization results are dominated by line polarization. To explain the required grain alignment, grain mineralogy effects, due to either fossil silicate grains from the earlier oxygen-rich AGB phase of the star or due to the incorporation of ferromagnetic inclusions in the largest grains, may play a role. We argue that the most likely explanation is due to a new alignment mechanism wherein a charged grain, moving relative to the magnetic field, precesses around the induced electric field and therefore aligns with the magnetic field. This mechanism is particularly attractive as the optical, FIR, and submillimeter-wave polarization of the carbon dust can then be explained in a consistent way, differing simply due to the charge state of the grains. Circumstellar dust Magnetic fields Carbonaceous grains Asymptotic giant branch stars Astrophysics Janik Karoly verfasserin aut Pierre Bastien verfasserin aut Archana Soam verfasserin aut Simon Coudé verfasserin aut Mehrnoosh Tahani verfasserin aut Michael S. Gordon verfasserin aut Sydney Fox-Middleton verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 963(2024), 1, p 76 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:963 year:2024 number:1, p 76 https://doi.org/10.3847/1538-4357/ad1835 kostenfrei https://doaj.org/article/6664fa8bb6be44029f141a001e2f82a5 kostenfrei https://doi.org/10.3847/1538-4357/ad1835 kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 963 2024 1, p 76
spelling	10.3847/1538-4357/ad1835 doi (DE-627)DOAJ10165586X (DE-599)DOAJ6664fa8bb6be44029f141a001e2f82a5 DE-627 ger DE-627 rakwb eng QB460-466 B-G. Andersson verfasserin aut Submillimeter-wavelength Polarimetry of IRC+10216 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present SCUBA-2/POL-2 850 μ m polarimetric observations of the circumstellar envelope (CSE) of the carbon-rich asymptotic giant branch (AGB) star IRC+10216. Both far-IR (FIR) and optical polarization data indicate grains aligned with their long axis in the radial direction relative to the central star. The 850 μ m polarization does not show this simple structure. The 850 μ m data are indicative, albeit not conclusive, of a magnetic dipole geometry. Assuming such a simple dipole geometry, the resulting 850 μ m polarization geometry is consistent with both Zeeman observations and small-scale structure in the CSE. While there is significant spectral-line polarization contained within the SCUBA-2 850 μ m passband for the source, it is unlikely that our broadband polarization results are dominated by line polarization. To explain the required grain alignment, grain mineralogy effects, due to either fossil silicate grains from the earlier oxygen-rich AGB phase of the star or due to the incorporation of ferromagnetic inclusions in the largest grains, may play a role. We argue that the most likely explanation is due to a new alignment mechanism wherein a charged grain, moving relative to the magnetic field, precesses around the induced electric field and therefore aligns with the magnetic field. This mechanism is particularly attractive as the optical, FIR, and submillimeter-wave polarization of the carbon dust can then be explained in a consistent way, differing simply due to the charge state of the grains. Circumstellar dust Magnetic fields Carbonaceous grains Asymptotic giant branch stars Astrophysics Janik Karoly verfasserin aut Pierre Bastien verfasserin aut Archana Soam verfasserin aut Simon Coudé verfasserin aut Mehrnoosh Tahani verfasserin aut Michael S. Gordon verfasserin aut Sydney Fox-Middleton verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 963(2024), 1, p 76 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:963 year:2024 number:1, p 76 https://doi.org/10.3847/1538-4357/ad1835 kostenfrei https://doaj.org/article/6664fa8bb6be44029f141a001e2f82a5 kostenfrei https://doi.org/10.3847/1538-4357/ad1835 kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 963 2024 1, p 76
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allfieldsSound	10.3847/1538-4357/ad1835 doi (DE-627)DOAJ10165586X (DE-599)DOAJ6664fa8bb6be44029f141a001e2f82a5 DE-627 ger DE-627 rakwb eng QB460-466 B-G. Andersson verfasserin aut Submillimeter-wavelength Polarimetry of IRC+10216 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present SCUBA-2/POL-2 850 μ m polarimetric observations of the circumstellar envelope (CSE) of the carbon-rich asymptotic giant branch (AGB) star IRC+10216. Both far-IR (FIR) and optical polarization data indicate grains aligned with their long axis in the radial direction relative to the central star. The 850 μ m polarization does not show this simple structure. The 850 μ m data are indicative, albeit not conclusive, of a magnetic dipole geometry. Assuming such a simple dipole geometry, the resulting 850 μ m polarization geometry is consistent with both Zeeman observations and small-scale structure in the CSE. While there is significant spectral-line polarization contained within the SCUBA-2 850 μ m passband for the source, it is unlikely that our broadband polarization results are dominated by line polarization. To explain the required grain alignment, grain mineralogy effects, due to either fossil silicate grains from the earlier oxygen-rich AGB phase of the star or due to the incorporation of ferromagnetic inclusions in the largest grains, may play a role. We argue that the most likely explanation is due to a new alignment mechanism wherein a charged grain, moving relative to the magnetic field, precesses around the induced electric field and therefore aligns with the magnetic field. This mechanism is particularly attractive as the optical, FIR, and submillimeter-wave polarization of the carbon dust can then be explained in a consistent way, differing simply due to the charge state of the grains. Circumstellar dust Magnetic fields Carbonaceous grains Asymptotic giant branch stars Astrophysics Janik Karoly verfasserin aut Pierre Bastien verfasserin aut Archana Soam verfasserin aut Simon Coudé verfasserin aut Mehrnoosh Tahani verfasserin aut Michael S. Gordon verfasserin aut Sydney Fox-Middleton verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 963(2024), 1, p 76 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:963 year:2024 number:1, p 76 https://doi.org/10.3847/1538-4357/ad1835 kostenfrei https://doaj.org/article/6664fa8bb6be44029f141a001e2f82a5 kostenfrei https://doi.org/10.3847/1538-4357/ad1835 kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 963 2024 1, p 76
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callnumber-first	Q - Science
author	B-G. Andersson
spellingShingle	B-G. Andersson misc QB460-466 misc Circumstellar dust misc Magnetic fields misc Carbonaceous grains misc Asymptotic giant branch stars misc Astrophysics Submillimeter-wavelength Polarimetry of IRC+10216
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topic_title	QB460-466 Submillimeter-wavelength Polarimetry of IRC+10216 Circumstellar dust Magnetic fields Carbonaceous grains Asymptotic giant branch stars
topic	misc QB460-466 misc Circumstellar dust misc Magnetic fields misc Carbonaceous grains misc Asymptotic giant branch stars misc Astrophysics
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title	Submillimeter-wavelength Polarimetry of IRC+10216
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title_sort	submillimeter-wavelength polarimetry of irc+10216
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title_auth	Submillimeter-wavelength Polarimetry of IRC+10216
abstract	We present SCUBA-2/POL-2 850 μ m polarimetric observations of the circumstellar envelope (CSE) of the carbon-rich asymptotic giant branch (AGB) star IRC+10216. Both far-IR (FIR) and optical polarization data indicate grains aligned with their long axis in the radial direction relative to the central star. The 850 μ m polarization does not show this simple structure. The 850 μ m data are indicative, albeit not conclusive, of a magnetic dipole geometry. Assuming such a simple dipole geometry, the resulting 850 μ m polarization geometry is consistent with both Zeeman observations and small-scale structure in the CSE. While there is significant spectral-line polarization contained within the SCUBA-2 850 μ m passband for the source, it is unlikely that our broadband polarization results are dominated by line polarization. To explain the required grain alignment, grain mineralogy effects, due to either fossil silicate grains from the earlier oxygen-rich AGB phase of the star or due to the incorporation of ferromagnetic inclusions in the largest grains, may play a role. We argue that the most likely explanation is due to a new alignment mechanism wherein a charged grain, moving relative to the magnetic field, precesses around the induced electric field and therefore aligns with the magnetic field. This mechanism is particularly attractive as the optical, FIR, and submillimeter-wave polarization of the carbon dust can then be explained in a consistent way, differing simply due to the charge state of the grains.
abstractGer	We present SCUBA-2/POL-2 850 μ m polarimetric observations of the circumstellar envelope (CSE) of the carbon-rich asymptotic giant branch (AGB) star IRC+10216. Both far-IR (FIR) and optical polarization data indicate grains aligned with their long axis in the radial direction relative to the central star. The 850 μ m polarization does not show this simple structure. The 850 μ m data are indicative, albeit not conclusive, of a magnetic dipole geometry. Assuming such a simple dipole geometry, the resulting 850 μ m polarization geometry is consistent with both Zeeman observations and small-scale structure in the CSE. While there is significant spectral-line polarization contained within the SCUBA-2 850 μ m passband for the source, it is unlikely that our broadband polarization results are dominated by line polarization. To explain the required grain alignment, grain mineralogy effects, due to either fossil silicate grains from the earlier oxygen-rich AGB phase of the star or due to the incorporation of ferromagnetic inclusions in the largest grains, may play a role. We argue that the most likely explanation is due to a new alignment mechanism wherein a charged grain, moving relative to the magnetic field, precesses around the induced electric field and therefore aligns with the magnetic field. This mechanism is particularly attractive as the optical, FIR, and submillimeter-wave polarization of the carbon dust can then be explained in a consistent way, differing simply due to the charge state of the grains.
abstract_unstemmed	We present SCUBA-2/POL-2 850 μ m polarimetric observations of the circumstellar envelope (CSE) of the carbon-rich asymptotic giant branch (AGB) star IRC+10216. Both far-IR (FIR) and optical polarization data indicate grains aligned with their long axis in the radial direction relative to the central star. The 850 μ m polarization does not show this simple structure. The 850 μ m data are indicative, albeit not conclusive, of a magnetic dipole geometry. Assuming such a simple dipole geometry, the resulting 850 μ m polarization geometry is consistent with both Zeeman observations and small-scale structure in the CSE. While there is significant spectral-line polarization contained within the SCUBA-2 850 μ m passband for the source, it is unlikely that our broadband polarization results are dominated by line polarization. To explain the required grain alignment, grain mineralogy effects, due to either fossil silicate grains from the earlier oxygen-rich AGB phase of the star or due to the incorporation of ferromagnetic inclusions in the largest grains, may play a role. We argue that the most likely explanation is due to a new alignment mechanism wherein a charged grain, moving relative to the magnetic field, precesses around the induced electric field and therefore aligns with the magnetic field. This mechanism is particularly attractive as the optical, FIR, and submillimeter-wave polarization of the carbon dust can then be explained in a consistent way, differing simply due to the charge state of the grains.
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title_short	Submillimeter-wavelength Polarimetry of IRC+10216
url	https://doi.org/10.3847/1538-4357/ad1835 https://doaj.org/article/6664fa8bb6be44029f141a001e2f82a5 https://doaj.org/toc/1538-4357
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up_date	2024-07-03T21:47:52.166Z
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Submillimeter-wavelength Polarimetry of IRC+10216

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