High degree solar oscillations in 3D numerical simulations

Dali Georgobiani; Robert F. Stein; Åke Nordlund; Alexander Kosovichev; Nagi N. Mansour

High degree solar oscillations in 3D numerical simulations

Dali Georgobiani, Robert F. Stein, Åke Nordlund, Alexander Kosovichev, Nagi N. Mansour

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

Abstract

Realistic 3D numerical simulations of solar convection are capable of reproducing the excitation of solar oscillations by turbulent convection. Continuing our investigations, we calculate velocity power spectra for high angular degree modes that have their lower turning points within the shallow simulation domain. We find excellent agreement between the observed SOHO/MDI and simulated power spectra in frequency, amplitude and mode width. However, surprisingly at lower frequencies, the noise level in the model is much higher than in the Sun.

Original language	English (US)
Pages (from-to)	267-270
Number of pages	4
Journal	European Space Agency, (Special Publication) ESA SP
Issue number	559
State	Published - Dec 1 2004
Externally published	Yes

All Science Journal Classification (ASJC) codes

Aerospace Engineering

Cite this

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title = "High degree solar oscillations in 3D numerical simulations",

abstract = "Realistic 3D numerical simulations of solar convection are capable of reproducing the excitation of solar oscillations by turbulent convection. Continuing our investigations, we calculate velocity power spectra for high angular degree modes that have their lower turning points within the shallow simulation domain. We find excellent agreement between the observed SOHO/MDI and simulated power spectra in frequency, amplitude and mode width. However, surprisingly at lower frequencies, the noise level in the model is much higher than in the Sun.",

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AU - Georgobiani, Dali

AU - Stein, Robert F.

AU - Nordlund, Åke

AU - Kosovichev, Alexander

AU - Mansour, Nagi N.

PY - 2004/12/1

Y1 - 2004/12/1

N2 - Realistic 3D numerical simulations of solar convection are capable of reproducing the excitation of solar oscillations by turbulent convection. Continuing our investigations, we calculate velocity power spectra for high angular degree modes that have their lower turning points within the shallow simulation domain. We find excellent agreement between the observed SOHO/MDI and simulated power spectra in frequency, amplitude and mode width. However, surprisingly at lower frequencies, the noise level in the model is much higher than in the Sun.

AB - Realistic 3D numerical simulations of solar convection are capable of reproducing the excitation of solar oscillations by turbulent convection. Continuing our investigations, we calculate velocity power spectra for high angular degree modes that have their lower turning points within the shallow simulation domain. We find excellent agreement between the observed SOHO/MDI and simulated power spectra in frequency, amplitude and mode width. However, surprisingly at lower frequencies, the noise level in the model is much higher than in the Sun.

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High degree solar oscillations in 3D numerical simulations

Abstract

All Science Journal Classification (ASJC) codes

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