Most detects g-modes in the late-type Be star β canis minoris (B8 Ve)

H. Saio; C. Cameron; R. Kuschnig; G. A.H. Walker; J. M. Matthews; J. F. Rowe; U. Lee; D. Huber; W. W. Weiss; D. B. Guenther; A. F.J. Moffat; S. M. Rucinski; D. Sasselov

doi:10.1086/509315

Most detects g-modes in the late-type Be star β canis minoris (B8 Ve)

H. Saio, C. Cameron, R. Kuschnig, G. A.H. Walker, J. M. Matthews, J. F. Rowe, U. Lee, D. Huber, W. W. Weiss, D. B. Guenther, A. F.J. Moffat, S. M. Rucinski, D. Sasselov

Research output: Contribution to journal › Article › peer-review

42 Citations (Scopus)

Abstract

The Microvariability and Oscillations of Stars (MOST) satellite has detected low-amplitude light variations (Δm ∼ 1 mmag) in the Be star β CMi (B8 Ve). The observations lasted 41 days and the variations have typical periods ∼0.3 days. We demonstrate that the dominant frequencies are consistent with prograde high-order g-modes of m = -1 excited by the Fe bump of opacity in an intermediate-mass (≈3.5 M_⊙) star with a nearly critical rotation period of 0.38 days. This is the first detection of nonradial g-mode pulsations in a Be star later than B6 leading to the possibility that pulsations are excited in all classical Be stars.

Original language	English
Pages (from-to)	544-550
Number of pages	7
Journal	Astrophysical Journal
Volume	654
Issue number	1 I
DOIs	https://doi.org/10.1086/509315
Publication status	Published - 2007 Jan 1

Keywords

Stars: early-type
Stars: emission-line, Be
Stars: individual (β Canis Minoris)
Stars: oscillations
Stars: rotation

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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Most detects g-modes in the late-type Be star β canis minoris (B8 Ve). / Saio, H.; Cameron, C.; Kuschnig, R.; Walker, G. A.H.; Matthews, J. M.; Rowe, J. F.; Lee, U.; Huber, D.; Weiss, W. W.; Guenther, D. B.; Moffat, A. F.J.; Rucinski, S. M.; Sasselov, D.

In: Astrophysical Journal, Vol. 654, No. 1 I, 01.01.2007, p. 544-550.

Research output: Contribution to journal › Article › peer-review

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abstract = "The Microvariability and Oscillations of Stars (MOST) satellite has detected low-amplitude light variations (Δm ∼ 1 mmag) in the Be star β CMi (B8 Ve). The observations lasted 41 days and the variations have typical periods ∼0.3 days. We demonstrate that the dominant frequencies are consistent with prograde high-order g-modes of m = -1 excited by the Fe bump of opacity in an intermediate-mass (≈3.5 M⊙) star with a nearly critical rotation period of 0.38 days. This is the first detection of nonradial g-mode pulsations in a Be star later than B6 leading to the possibility that pulsations are excited in all classical Be stars.",

keywords = "Stars: early-type, Stars: emission-line, Be, Stars: individual (β Canis Minoris), Stars: oscillations, Stars: rotation",

author = "H. Saio and C. Cameron and R. Kuschnig and Walker, {G. A.H.} and Matthews, {J. M.} and Rowe, {J. F.} and U. Lee and D. Huber and Weiss, {W. W.} and Guenther, {D. B.} and Moffat, {A. F.J.} and Rucinski, {S. M.} and D. Sasselov",

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AU - Saio, H.

AU - Cameron, C.

AU - Kuschnig, R.

AU - Walker, G. A.H.

AU - Matthews, J. M.

AU - Rowe, J. F.

AU - Lee, U.

AU - Huber, D.

AU - Weiss, W. W.

AU - Guenther, D. B.

AU - Moffat, A. F.J.

AU - Rucinski, S. M.

AU - Sasselov, D.

PY - 2007/1/1

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N2 - The Microvariability and Oscillations of Stars (MOST) satellite has detected low-amplitude light variations (Δm ∼ 1 mmag) in the Be star β CMi (B8 Ve). The observations lasted 41 days and the variations have typical periods ∼0.3 days. We demonstrate that the dominant frequencies are consistent with prograde high-order g-modes of m = -1 excited by the Fe bump of opacity in an intermediate-mass (≈3.5 M⊙) star with a nearly critical rotation period of 0.38 days. This is the first detection of nonradial g-mode pulsations in a Be star later than B6 leading to the possibility that pulsations are excited in all classical Be stars.

AB - The Microvariability and Oscillations of Stars (MOST) satellite has detected low-amplitude light variations (Δm ∼ 1 mmag) in the Be star β CMi (B8 Ve). The observations lasted 41 days and the variations have typical periods ∼0.3 days. We demonstrate that the dominant frequencies are consistent with prograde high-order g-modes of m = -1 excited by the Fe bump of opacity in an intermediate-mass (≈3.5 M⊙) star with a nearly critical rotation period of 0.38 days. This is the first detection of nonradial g-mode pulsations in a Be star later than B6 leading to the possibility that pulsations are excited in all classical Be stars.

KW - Stars: early-type

KW - Stars: emission-line, Be

KW - Stars: individual (β Canis Minoris)

KW - Stars: oscillations

KW - Stars: rotation

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