E-Print Archive

There are 4035 abstracts currently viewable.


Advanced Search
Main Page Add New E-Print Submitter
News Help/FAQ About Preferences
Manage Key Phrase
Constraining the Angular Momentum of the Sun with Planetary Orbital Motions and General Relativity View all abstracts by submitter

Lorenzo Iorio   Submitted: 2012-07-18 16:30

The angular momentum of a star is an important astrophysical quantityrelated to its internal structure, formation and evolution. Onaverage, helioseismology yields S = 1.92 x1041 kg m2 s-1 for the angularmomentum of the Sun. We show how it should be possible to measure or,at least, constrain it in a near future by using the gravitomagneticLense-Thirring effect predicted by general relativity for the orbit ofa test particle moving around a central rotating body. We also discussthe present-day situation in view of the latest determinations of thesupplementary perihelion precession of Mercury. A fit by Fienga et al.(Celestial Mech. Dynamical Astron. 111, 363, 2011) of the dynamicalmodels of several standard forces acting on the planets of the solarsystem to a long data record yielded 0.4 ± 0.6 milliarcseconds percentury. The modeled forces did not include the Lense-Thirring effectitself, which is expected to be as large as -2.0 milliarcseconds percentury.from helioseismology-based values of S. By assuming thevalidity of General Relativity, from its theoretical prediction forthe gravitomagnetic perihelion precession of Mercury one canstraightforwardly infer S <= 0.95 x1041 kg m2 s-1. It disagrees with thecurrently available values from helioseismology. Possible sources forthe present discrepancy are examined. Given the current level ofaccuracy in the Mercury ephemerides, the gravitomagnetic force of theSun should be included in their force models. MESSENGER, in orbitaround Mercury since March 2011, will collect science data until 2013,while BepiColombo, to be launched in 2015, should reach Mercury in2022 for a year-long science phase: the analysis of their data will beimportant in eectively constraining S in about a decade or, perhaps,even less.

Authors: Lorenzo Iorio
Projects: Other

Publication Status: To appear in Solar Physics
Last Modified: 2012-07-19 11:53
Go to main E-Print page  Generation of Large Scale Electric Fields in Coronal Flare Circuits  Self-Organized Criticality Systems in Astrophysics (Chapter 13)  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

Go to main E-Print pageGo to main E-Print page.
Previous AbstractPrevious Abstract.
Next AbstractNext Abstract.
Download PreprintDownload Preprint.
Submitter's HomepageSubmitters Homepage.
Edit EntryEdit Entry.
View All Abstracts By SubmitterView all abstracts by submitter.
Delete AbstractDelete abstract.

Latest Entries
Why Does the Solar Corona Abnormally Rotate Faster Than the Photosphere?
Impacts On Proton Fluxes Observed During Different Interplanetary Conditions
Coronal Loop Seismology Using Standing Kink Oscillations With a Lookup Table
Data-Optimized Coronal Field Model: I. Proof of Concept
Coronal Bright Points
Difference of source regions between fast and slow coronal mass ejections
Invited Review: Signatures of Magnetic Flux Ropes in the Low Solar Atmosphere Observed in High Resolution
Do Kepler superflare stars really include slowly-rotating Sun-like stars ? - Results using APO 3.5m telescope spectroscopic observations and Gaia-DR2 data -
Magnetically Induced Current Piston for Generating Extreme-ultraviolet Fronts in the Solar Corona
Magnetic Field Dynamics and Varying Plasma Emission in Large-scale Coronal Loops
Nonlinear Evolution of Ion Kinetic Instabilities in the Solar Wind
What determines the X-ray intensity and duration of a solar flare?
Fast Magnetoacoustic Wave Trains with Time-dependent Drivers
Three-dimensional reconstruction of CME-driven shock-streamer interaction from radio observations: a different take on the diagnostics of coronal magnetic fields
The soft X-ray spectrometer polarimeter SolpeX
Variable emission mechanism of a Type IV radio burst
Inference of magnetic field strength and density from damped transverse coronal waves
Frequency-Distance Structure of Solar Radio Sources Observed by LOFAR
The birth of a coronal mass ejection
Properties of slow magnetoacoustic oscillations of solar coronal loops by multi-instrumental observations

Related Pages
MSU Solar Physics.
Max Millennium Science Mail Archive.
Max Millennium Message of the Day Mail Archive.
Max Millennium Flare Catalog

Archive Maintainer
Alisdair Davey

© 2003 Solar Physics Group - Montana State University