2024-09-24T22:21:26.000Z http://sot.lmsal.com Mr. Sam Freeland Lockheed Martin Solar and Astrophysics Laboratory (LMSAL) http://www.lmsal.com Lockheed Martin Advanced Tech Center, 3251 Hanover Rd, O/ADBS, B/252, Palo Alto, CA 94304 null null HINODE SOTSP Arikawa Sterling Suematsu 72 HOP 72 Quiet Sun Radiative structure of small magnetic elements: faculae, network and inter network in the quiet Sun QS 7 20080808_093043 186 209 222 7 68 384 2 1 1 2 0 22 2021 162 0.84375 -517.604 -0.672 51.354 81.152 2008-08-08T09:30:43.000Z 2008-08-08T09:40:56.000Z -517.604 -0.672 Radiative structure of small magnetic elements: faculae, network and inter network in the quiet Sun Fast map, 62"x82", single, 1-side CCD, Q75 Scientific Objectives: The smallest magnetic features in the solar photosphere are the G-band bright points. It is fundamental to study their structure and size, as they are in the resolution limit,and can appear as points or unresolved features (Ishiwawa et al 2007, Berger et al 2004). We intend to study them at maximum spatial resolution in intensity and magnetic field at several wavelengths to determine their dimensional and thermal structure. Observations in G-band (=430.5nm), CaII(=396.9nm), CN(=388.35nm) as well as magnetograms: MgIb(=517.27nm), FeI(=517.27nm) and NaID(=589.6nm are proposed in this document.;;Scientific Objectives: The smallest magnetic features in the solar photosphere are the G-band bright points. It is fundamental to study their structure and size, as they are in the resolution limit,and can appear as points or unresolved features (Ishiwawa et al 2007, Berger et al 2004). We intend to study them at maximum spatial resolution in intensity and magnetic field at several wavelengths to determine their dimensional and thermal structure. Observations in G-band (=430.5nm), CaII(=396.9nm), CN(=388.35nm) as well as magnetograms: MgIb(=517.27nm), FeI(=517.27nm) and NaID(=589.6nm are proposed in this document. ivo://sot.lmsal.com/VOEvent#2008-08-08T09:30:00Z