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Table 1.

Recent results of the solar radius at 1 au using different methods and instruments for different wavelength ().

Author(s) Dates Method (instrument) (nm) STD (km) (km)
Vaquero et al. (2016) 1773–2006 Transit times (several instruments) 695 438 1284
Lamy et al. (2015) 2010–2015 Total solar eclipses (photometers) 540.00 696 251 15

Sofia et al. (2013) 1992–2011 Prism as angular reference (sextant) 615.00 695 997 696 171 15

Emilio et al. (2012) 2003 and 2006 Mercury transits (MDI) 676.78 696 345 65
Hauchecorne et al. (2014) 2012 Venus transit (HMI) 617.30 696 185 44
Meftah et al. (2014b) 2012 Venus transit (SODISM) 607.10 696 156 44 145
Emilio et al. (2015) 2012 Venus transit (HMI) 617.30 695 946 15

IAU () 2015 Transit and helioseismic determinations 695 700

Notes. Solar radius measurements using the transit-timing method, Vaquero et al. (2016) ground-based measurements made in the Royal Observatory of the Spanish Navy; prism angular reference, Solar Disk Sextant (SDS) balloon flights; planet transits, the Michelson Doppler Imager (MDI) on board the Solar and Heliospheric Observatory, the Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory, SODISM on board PICARD; and solar eclipses, ground-based measurements made with solar photometers. STD represents the standard error, which depicts the dispersion of individual observations around the mean or median value. is the combined standard uncertainty of the individual standard uncertainties (errors of the uncertainty budget). For example, the typical estimated uncertainty of each SDS measurement (Sofia et al. 2013) is 15 km (0.02 arcsec) with a solar radius that is found to vary by up to 174 km (real variation and/or error) from 1992 to 2011.

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