Simulating the outer layers of Procyon A

A comparison with the Sun

F. J. Robinson, P. Demarque, D. B. Guenther, Yong Cheol Kim, K. L. Chan

Research output: Contribution to journalReview article

16 Citations (Scopus)

Abstract

We compare a new 3D radiative hydrodynamical simulation of the surface layers of Procyon A to a similar 3D simulation of the surface layers of the Sun. Both simulations include realistic input physics and are performed using the same numerical techniques and computer codes. Convection in the surface layers of Procyon A is very different from the Sun. Compared with the Sun, the atmospheric structure and convective flow in Procyon A exhibit the following characteristics. (i)The highly superadiabatic transition layer (SAL) is located at a much shallower optical depth; it is in a dynamically active region and its outer region is sometimes located in the optically thin atmosphere. (ii)The outer region of the SAL moves from an optically thin region to a thick region and back again over a time of 20-30 min. This motion, which is driven by the granulation, takes place in a time approximately half the turnover time of the largest granules. (iii)The peak rms velocity in the vertical direction is much larger in Procyon A. The main reason for the radically different radiative-convective behaviour in Procyon A compared with the Sun is the role played by turbulent eddies in determining the overall flow/thermal structure. The turbulent pressure and turbulent kinetic energy can exceed 50 per cent of the local gas pressure (compared with about 10-20 per cent in the Sun). In such regions, the mixing lengthy theory is a poor approximation. The Procyon A simulation thus reveals two distinct time-scales: the autocorrelation time of the vertical velocity and the characteristic time-scale of the SAL, which is tied to granulation. Just below the surface, the autocorrelation decay time is about 5 min in Procyon A and the SAL motion time-scale is 20-30 min. In the simulations, the peak value of the superadiabaticity varies between 0.5 and 3. When the SAL penetrates the optically thin region, there are efficient radiative losses and the peak of the SAL is low. We speculate that these losses damp out the relative amplitudes in luminosity (temperature fluctuations) compared with velocity (Doppler). Although this will not affect the frequencies of the peaks in the power spectrum, it will probably lower the average amplitude of the peaks relative to the noise background.

Original languageEnglish
Pages (from-to)1031-1037
Number of pages7
JournalMonthly Notices of the Royal Astronomical Society
Volume362
Issue number3
DOIs
Publication statusPublished - 2005 Sep 21

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transition layers
sun
surface layer
simulation
surface layers
timescale
autocorrelation
atmospheric structure
thermal structure
comparison
convective flow
background noise
optical depth
kinetic energy
eddy
turnover
optical thickness
physics
gas pressure
power spectra

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Robinson, F. J. ; Demarque, P. ; Guenther, D. B. ; Kim, Yong Cheol ; Chan, K. L. / Simulating the outer layers of Procyon A : A comparison with the Sun. In: Monthly Notices of the Royal Astronomical Society. 2005 ; Vol. 362, No. 3. pp. 1031-1037.
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abstract = "We compare a new 3D radiative hydrodynamical simulation of the surface layers of Procyon A to a similar 3D simulation of the surface layers of the Sun. Both simulations include realistic input physics and are performed using the same numerical techniques and computer codes. Convection in the surface layers of Procyon A is very different from the Sun. Compared with the Sun, the atmospheric structure and convective flow in Procyon A exhibit the following characteristics. (i)The highly superadiabatic transition layer (SAL) is located at a much shallower optical depth; it is in a dynamically active region and its outer region is sometimes located in the optically thin atmosphere. (ii)The outer region of the SAL moves from an optically thin region to a thick region and back again over a time of 20-30 min. This motion, which is driven by the granulation, takes place in a time approximately half the turnover time of the largest granules. (iii)The peak rms velocity in the vertical direction is much larger in Procyon A. The main reason for the radically different radiative-convective behaviour in Procyon A compared with the Sun is the role played by turbulent eddies in determining the overall flow/thermal structure. The turbulent pressure and turbulent kinetic energy can exceed 50 per cent of the local gas pressure (compared with about 10-20 per cent in the Sun). In such regions, the mixing lengthy theory is a poor approximation. The Procyon A simulation thus reveals two distinct time-scales: the autocorrelation time of the vertical velocity and the characteristic time-scale of the SAL, which is tied to granulation. Just below the surface, the autocorrelation decay time is about 5 min in Procyon A and the SAL motion time-scale is 20-30 min. In the simulations, the peak value of the superadiabaticity varies between 0.5 and 3. When the SAL penetrates the optically thin region, there are efficient radiative losses and the peak of the SAL is low. We speculate that these losses damp out the relative amplitudes in luminosity (temperature fluctuations) compared with velocity (Doppler). Although this will not affect the frequencies of the peaks in the power spectrum, it will probably lower the average amplitude of the peaks relative to the noise background.",
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Simulating the outer layers of Procyon A : A comparison with the Sun. / Robinson, F. J.; Demarque, P.; Guenther, D. B.; Kim, Yong Cheol; Chan, K. L.

In: Monthly Notices of the Royal Astronomical Society, Vol. 362, No. 3, 21.09.2005, p. 1031-1037.

Research output: Contribution to journalReview article

TY - JOUR

T1 - Simulating the outer layers of Procyon A

T2 - A comparison with the Sun

AU - Robinson, F. J.

AU - Demarque, P.

AU - Guenther, D. B.

AU - Kim, Yong Cheol

AU - Chan, K. L.

PY - 2005/9/21

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N2 - We compare a new 3D radiative hydrodynamical simulation of the surface layers of Procyon A to a similar 3D simulation of the surface layers of the Sun. Both simulations include realistic input physics and are performed using the same numerical techniques and computer codes. Convection in the surface layers of Procyon A is very different from the Sun. Compared with the Sun, the atmospheric structure and convective flow in Procyon A exhibit the following characteristics. (i)The highly superadiabatic transition layer (SAL) is located at a much shallower optical depth; it is in a dynamically active region and its outer region is sometimes located in the optically thin atmosphere. (ii)The outer region of the SAL moves from an optically thin region to a thick region and back again over a time of 20-30 min. This motion, which is driven by the granulation, takes place in a time approximately half the turnover time of the largest granules. (iii)The peak rms velocity in the vertical direction is much larger in Procyon A. The main reason for the radically different radiative-convective behaviour in Procyon A compared with the Sun is the role played by turbulent eddies in determining the overall flow/thermal structure. The turbulent pressure and turbulent kinetic energy can exceed 50 per cent of the local gas pressure (compared with about 10-20 per cent in the Sun). In such regions, the mixing lengthy theory is a poor approximation. The Procyon A simulation thus reveals two distinct time-scales: the autocorrelation time of the vertical velocity and the characteristic time-scale of the SAL, which is tied to granulation. Just below the surface, the autocorrelation decay time is about 5 min in Procyon A and the SAL motion time-scale is 20-30 min. In the simulations, the peak value of the superadiabaticity varies between 0.5 and 3. When the SAL penetrates the optically thin region, there are efficient radiative losses and the peak of the SAL is low. We speculate that these losses damp out the relative amplitudes in luminosity (temperature fluctuations) compared with velocity (Doppler). Although this will not affect the frequencies of the peaks in the power spectrum, it will probably lower the average amplitude of the peaks relative to the noise background.

AB - We compare a new 3D radiative hydrodynamical simulation of the surface layers of Procyon A to a similar 3D simulation of the surface layers of the Sun. Both simulations include realistic input physics and are performed using the same numerical techniques and computer codes. Convection in the surface layers of Procyon A is very different from the Sun. Compared with the Sun, the atmospheric structure and convective flow in Procyon A exhibit the following characteristics. (i)The highly superadiabatic transition layer (SAL) is located at a much shallower optical depth; it is in a dynamically active region and its outer region is sometimes located in the optically thin atmosphere. (ii)The outer region of the SAL moves from an optically thin region to a thick region and back again over a time of 20-30 min. This motion, which is driven by the granulation, takes place in a time approximately half the turnover time of the largest granules. (iii)The peak rms velocity in the vertical direction is much larger in Procyon A. The main reason for the radically different radiative-convective behaviour in Procyon A compared with the Sun is the role played by turbulent eddies in determining the overall flow/thermal structure. The turbulent pressure and turbulent kinetic energy can exceed 50 per cent of the local gas pressure (compared with about 10-20 per cent in the Sun). In such regions, the mixing lengthy theory is a poor approximation. The Procyon A simulation thus reveals two distinct time-scales: the autocorrelation time of the vertical velocity and the characteristic time-scale of the SAL, which is tied to granulation. Just below the surface, the autocorrelation decay time is about 5 min in Procyon A and the SAL motion time-scale is 20-30 min. In the simulations, the peak value of the superadiabaticity varies between 0.5 and 3. When the SAL penetrates the optically thin region, there are efficient radiative losses and the peak of the SAL is low. We speculate that these losses damp out the relative amplitudes in luminosity (temperature fluctuations) compared with velocity (Doppler). Although this will not affect the frequencies of the peaks in the power spectrum, it will probably lower the average amplitude of the peaks relative to the noise background.

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