UV, IR, and MM studies of CO surrounding the red supergiant α orionis (M2 Iab)

Graham M. Harper, Kenneth G. Carpenter, Nils Ryde, Nathan Smith, Joanna Brown, Alexander Brown, Kenneth H. Hinkle

Research output: Chapter in Book/Report/Conference proceedingConference contribution

3 Citations (Scopus)

Abstract

Carbon monoxide has been detected in Betelgeuse's ultraviolet (electronic), infrared (vibrational), and mm-radio (rotational) spectra, but its spatial distribution has remained elusive. We have obtained new mm-radio interferometry (CARMA), infrared spatially-resolved spectra (Phoenix/Gemini-South), and we have performed non-LTE simulations to help establish the spatial location of the S1 (V = 10km/s) and S2 (V = 17km/s) CO shells. The strong CO Fourth-Positive ultraviolet scattering signature is apparent in the HST GHRS G140L spectrum and the S1 and S2 shells account for much of the UV opacity. Phoenix spectra reveal that the low velocity S1 shell is present at 1.5arcsec West of the star and extends out to ∼4arcsec, and its mm-radio emission appears to originate within an 6 arcsec radius. The interpretation of the S2 shell is less clear. The Phoenix spectra tentatively suggest that the S2 shell extends to ∼7 arcsec. The CARMA channel maps show an additional strong narrow emission component 5 arcsec from the star, but the spectra do not show all the expected S1 and S2 signatures. Future CARMA observations should help to disentangle the signature of the S1 and S2 shells.

Original languageEnglish (US)
Title of host publicationAIP Conference Proceedings
Pages868-871
Number of pages4
Volume1094
DOIs
StatePublished - 2009
Externally publishedYes
Event15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun - St. Andrews, United Kingdom
Duration: Jul 21 2008Jul 25 2008

Other

Other15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun
CountryUnited Kingdom
CitySt. Andrews
Period7/21/087/25/08

Fingerprint

Phoenix (AZ)
signatures
stars
radio spectra
rotational spectra
radio emission
opacity
carbon monoxide
low speed
spatial distribution
interferometry
radii
scattering
electronics
simulation

Keywords

  • α Orionis
  • Betelgeuse
  • Mass loss
  • Radiative transfer

ASJC Scopus subject areas

  • Physics and Astronomy(all)

Cite this

Harper, G. M., Carpenter, K. G., Ryde, N., Smith, N., Brown, J., Brown, A., & Hinkle, K. H. (2009). UV, IR, and MM studies of CO surrounding the red supergiant α orionis (M2 Iab). In AIP Conference Proceedings (Vol. 1094, pp. 868-871) https://doi.org/10.1063/1.3099254

UV, IR, and MM studies of CO surrounding the red supergiant α orionis (M2 Iab). / Harper, Graham M.; Carpenter, Kenneth G.; Ryde, Nils; Smith, Nathan; Brown, Joanna; Brown, Alexander; Hinkle, Kenneth H.

AIP Conference Proceedings. Vol. 1094 2009. p. 868-871.

Research output: Chapter in Book/Report/Conference proceedingConference contribution

Harper, GM, Carpenter, KG, Ryde, N, Smith, N, Brown, J, Brown, A & Hinkle, KH 2009, UV, IR, and MM studies of CO surrounding the red supergiant α orionis (M2 Iab). in AIP Conference Proceedings. vol. 1094, pp. 868-871, 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun, St. Andrews, United Kingdom, 7/21/08. https://doi.org/10.1063/1.3099254
Harper GM, Carpenter KG, Ryde N, Smith N, Brown J, Brown A et al. UV, IR, and MM studies of CO surrounding the red supergiant α orionis (M2 Iab). In AIP Conference Proceedings. Vol. 1094. 2009. p. 868-871 https://doi.org/10.1063/1.3099254
Harper, Graham M. ; Carpenter, Kenneth G. ; Ryde, Nils ; Smith, Nathan ; Brown, Joanna ; Brown, Alexander ; Hinkle, Kenneth H. / UV, IR, and MM studies of CO surrounding the red supergiant α orionis (M2 Iab). AIP Conference Proceedings. Vol. 1094 2009. pp. 868-871
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AU - Brown, Joanna

AU - Brown, Alexander

AU - Hinkle, Kenneth H.

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AB - Carbon monoxide has been detected in Betelgeuse's ultraviolet (electronic), infrared (vibrational), and mm-radio (rotational) spectra, but its spatial distribution has remained elusive. We have obtained new mm-radio interferometry (CARMA), infrared spatially-resolved spectra (Phoenix/Gemini-South), and we have performed non-LTE simulations to help establish the spatial location of the S1 (V = 10km/s) and S2 (V = 17km/s) CO shells. The strong CO Fourth-Positive ultraviolet scattering signature is apparent in the HST GHRS G140L spectrum and the S1 and S2 shells account for much of the UV opacity. Phoenix spectra reveal that the low velocity S1 shell is present at 1.5arcsec West of the star and extends out to ∼4arcsec, and its mm-radio emission appears to originate within an 6 arcsec radius. The interpretation of the S2 shell is less clear. The Phoenix spectra tentatively suggest that the S2 shell extends to ∼7 arcsec. The CARMA channel maps show an additional strong narrow emission component 5 arcsec from the star, but the spectra do not show all the expected S1 and S2 signatures. Future CARMA observations should help to disentangle the signature of the S1 and S2 shells.

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