Measurements of Solar Irradiance and Effective Temperature as a Probe of Solar Interior Magnetic Fields

Li, L. H.; Sofia, S.

doi:10.1086/319470

Cited by 31 publications

(29 citation statements)

References 17 publications

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“…As in the case of the ∼80 yr cycle, however, the results vary. The diameter appears to have changed either in phase with surface activity (Ulrich & Bertello 1995;Basu 1998;Emilio et al 2000;Noël 2004) or in antiphase with surface activity (Gilliland 1981;Sofia et al 1994;Laclare et al 1996;Li & Sofia 2001;Reis Neto et al 2003;Thuillier et al 2005;Egidi et al 2006). Some studies have detected no significant change at all (LaBonte & Howard 1981;Brown & Christensen-Dalsgaard 1998;Wittmann 2003;Kuhn et al 2004;Badache-Damiani & Rozelot 2006).…”

Section: ϫ3mentioning

confidence: 97%

A Virial Theorem Investigation of Magnetic Variations in the Sun

Stothers

2006

ApJ

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The magnetic virial theorem is applied here to a long-standing astrophysical problem, namely, the sign of the Sun's radius change during the solar activity cycle. The solar radius is theoretically found to decrease around the time of maximum magnetic field strength, in agreement with the best available observational evidence. This theoretical prediction, although simply based, instills some confidence by explicitly satisfying the conservation of total energy.

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Section: ϫ3mentioning

confidence: 97%

A Virial Theorem Investigation of Magnetic Variations in the Sun

Stothers

2006

ApJ

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“…Recent results for the Sun show that during the solar cycle structural adjustments in the solar interior are taking place which induce detectable changes of 0.1% in photospheric temperature and 0.02% in total irradiance. The changes in radius of the Sun are estimated to be of the order of 0.001% (Li & Sofia 2001). These detected changes of the solar parameters make it feasible that during a magnetic cycle changes in the global parameters of an RR Lyrae star may also occur.…”

Section: Magnetic Cyclesmentioning

confidence: 98%

“…Thanks to recent technical developments we have been able to learn more and more about the magnetic field structure and the 11-22-year magnetic cycle of the Sun. It is already well established that, as a consequence of changes in the global field strength and structure during the magnetic cycle, slight changes in most of the global solar parameters and also in both the p and f mode oscillationary frequencies are taking place (see e.g., Dziembowski et al 2001;Li & Sofia 2001;Zieba et al 2001).…”

Section: Magnetic Cyclesmentioning

confidence: 99%

Long-term photometric behaviour of XZ Dra

Jurcsik¹,

Benkő²,

Szeidl³

2002

A&A

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Abstract. The extended photometry available for XZ Dra, a Blazhko-type RR Lyrae star, makes it possible to study its longterm behavior. It is shown that its pulsation period exhibits cyclic, but not strictly regular variations with ≈7200 d period. The Blazhko period (≈76 d) seems to follow the observed period changes of the fundamental mode pulsation with dP B /dP 0 = 7.7 × 10 4 gradient. A binary model cannot explain this order of period change of the Blazhko modulation, nevertheless it can be brought into agreement with the O-C data of the pulsation. The possibility of occurrence of a magnetic cycle is raised.

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“…Following Li & Sofia (2001), we use the toroidal (B t ) and poloidal (B p ) components to express a magnetic field vector…”

Section: Proposed Solar Modelsmentioning

confidence: 99%

Solar Models With New Low metal Abundances

Yang

2016

ApJ

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In the past decade, the photospheric abundances of the Sun had been revised several times by many observers. The standard solar models constructed with the new low-metal abundances disagree with helioseismic results and detected neutrino fluxes. The solar model problem haspuzzled somestellar physicists for more than 10years. Rotation, enhanced diffusion, convection overshoot, and magnetic fields are used to reconcile the new abundances with helioseismology. The too lowhelium subsurface abundance in enhanced diffusion models can be improved by the mixing caused by rotation and magnetic fields. The problem of the depth of the convective zone in rotating models can be resolved by convection overshoot. Consequently, the Asplund-Grevesse-Sauval rotation model including overshooting (AGSR) reproduces the seismically inferred sound-speed and density profilesand the convection zone depth as well as the Grevesse & Sauval model computed before. But this model fails to reproduce the surface helium abundance, which is 0.2393 (2.6σ away from the seismic value), and neutrino fluxes. The magnetic model called AGSM keeps the agreement of the AGSR and improves the prediction of the surface helium abundance. The observed separation ratios r 02 and r 13 are reasonably reproduced by AGSM. Moreover, neutrino fluxes calculated by this model are not far from the detected neutrino fluxes and the predictions of previous works.

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Measurements of Solar Irradiance and Effective Temperature as a Probe of Solar Interior Magnetic Fields

Cited by 31 publications

References 17 publications

A Virial Theorem Investigation of Magnetic Variations in the Sun

A Virial Theorem Investigation of Magnetic Variations in the Sun

Long-term photometric behaviour of XZ Dra

Solar Models With New Low metal Abundances

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