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Rhodes, E. J.; Kosovichev, A. G.; Schou, J.; Scherrer, P. H.; Reiter, J.

doi:10.1023/a:1004963425123

Cited by 79 publications

(59 citation statements)

References 15 publications

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“…We find a higher sensitivity for the short-duration frequencies and confirm the findings of Rhodes, Reiter, and Schou (2003). However, we do not find any explanation for the results of Rose et al (2003) who could not confirm the higher value of sensitivity using GONG ++ data.…”

Section: Comparison With Standard Gong and MDI Datasupporting

confidence: 83%

“…However, there is still no consensus regarding the physical mechanism that gives rise to these changes (Kuhn, 2001). One deficiency is the lack of measurements for modes at high frequency and high degree (Rhodes, Reiter, and Schou, 2003) and little information about the correlation on short time scales. Since the p-mode frequency changes are thought to be associated with individual active regions that come and go continuously (Hindman et al, 2000), one would anticipate that the frequencies also change continuously on any time scale.…”

Section: Introductionmentioning

confidence: 99%

“…Thus, the use of mode frequencies and other parameters derived from short time series, during which the solar activity varies less, may help understand the underlying mechanism of these variations. Rhodes, Reiter, and Schou (2003) used a few sets of three-day time series in the computation and fitting of intermediate-degree p-mode frequencies and widths. The analysis, using Michelson Doppler Imager (MDI) and Mount Wilson Observatory (MWO) data, resulted in a higher sensitivity as measured from the slope of the linear regression between the frequency shifts and activity differences, compared to the slopes from longer time series.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Solar Oscillation Frequency Changes on Time Scales of Nine Days

Tripathy¹,

Hill²,

Jain³

et al. 2007

Sol Phys

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We establish that global solar p-mode frequencies can be measured with sufficient precision on time scales as short as nine days to detect activity-related shifts. Using ten years of GONG data, we report that mode-mass and error-weighted frequency shifts derived from nine days are significantly correlated with the strength of solar activity and are consistent with long-duration measurements from GONG and the SOHO/MDI instrument. The analysis of the year-wise distribution of the frequency shifts with change in activity indices shows that both the linear-regression slopes and the magnitude of the correlation varies from year to year and they are well correlated with each other. The study also indicates that the magnetic indices behave differently in the rising and falling phases of the activity cycle. For the short-duration nine-day observations, we report a higher sensitivity to activity.

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Section: Comparison With Standard Gong and MDI Datasupporting

confidence: 83%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Solar Oscillation Frequency Changes on Time Scales of Nine Days

Tripathy¹,

Hill²,

Jain³

et al. 2007

Sol Phys

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“…First, we add the depth of the solar convection zone R cz , followed by the helium abundance in the solar convection zone. Lastly, we consider the rms deviation of the model's sound speed profile δc s from that deduced from helioseismology (Rhodes et al 1997). The values used are given in Table 2.…”

Section: The Effects Of the Choice Of Solar Calibrationmentioning

confidence: 99%

Confronting uncertainties in stellar physics

Stancliffe

Fossati

Passy

et al. 2016

A&A

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We assess the systematic uncertainties in stellar evolutionary calculations for low-to intermediate-mass, main-sequence stars. We compare published stellar tracks from several different evolution codes with our own tracks computed using the stellar codes stars and mesa. In particular, we focus on tracks of 1 and 3 M at solar metallicity. We find that the spread in the available 1 M tracks (computed before the recent solar composition revision) can be covered by tracks between 0.97−1.01 M computed with the stars code. We assess some possible causes of the origin of this uncertainty, including how the choice of input physics and the solar constraints used to perform the solar calibration affect the tracks. We find that for a 1 M track, uncertainties of around 10% in the initial hydrogen abundance and initial metallicity produce around a 2% error in mass. For the 3 M tracks, there is very little difference between the tracks from the various different stellar codes. The main difference comes in the extent of the main sequence, which we believe results from the different choices of the implementation of convective overshooting in the core. Uncertainties in the initial abundances lead to a 1−2% error in the mass determination. These uncertainties cover only part of the total error budget, which should also include uncertainties in the input physics (e.g., reaction rates, opacities, convective models) and any missing physics (e.g., radiative levitation, rotation, magnetic fields). Uncertainties in stellar surface properties such as luminosity and effective temperature will further reduce the accuracy of any potential mass determinations.

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“…We use the frequencies of modes with , 1, 2 and l p 0 n ≤ proposed recently by García et al (2001) Bertello et al (2000b), l p 0-2 n 1 1.5 and of modes with from Rhodes et al (1997). (b) Similar inversions l p 3-300 after removal of modes with and .…”

Section: The Sound-speed Profilementioning

confidence: 99%

Solar Neutrino Emission Deduced from a Seismic Model

Turck‐Chièze¹,

Couvidat²,

Kosovichev³

et al. 2001

The Astrophysical Journal

165

152

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Three helioseismic instruments on the Solar and Heliospheric Observatory have observed the Sun almost continuously since early 1996. This has led to detailed study of the biases induced by the instruments that measure intensity or Doppler velocity variation. Photospheric turbulence hardly influences the tiny signature of conditions in the energy-generating core in the low-order modes, which are therefore very informative. We use sound-speed and density profiles inferred from GOLF and MDI data including these modes, together with recent improvements to stellar model computations, to build a spherically symmetric seismically adjusted model in agreement with the observations. The model is in hydrostatic and thermal balance and produces the present observed luminosity. In constructing the model, we adopt the best physics available, although we adjust some fundamental ingredients, well within the commonly estimated errors, such as the p-p reaction rate (ϩ1%) and the heavy-element abundance (ϩ3.5%); we also examine the sensitivity of the density profile to the nuclear reaction rates. Then, we deduce the corresponding emitted neutrino fluxes and consequently demonstrate that it is unlikely that the deficit of the neutrino fluxes measured on Earth can be explained by a spherically symmetric classical model without neutrino flavor transitions. Finally, we discuss the limitations of our results and future developments.

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Cited by 79 publications

References 15 publications

Solar Oscillation Frequency Changes on Time Scales of Nine Days

Solar Oscillation Frequency Changes on Time Scales of Nine Days

Confronting uncertainties in stellar physics

Solar Neutrino Emission Deduced from a Seismic Model

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