Experimental Detection of Thermal Radiation from Interplanetary Dust

Peterson, A. W.

doi:10.1086/180009

Cited by 73 publications

(15 citation statements)

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“…As might have been expected, Peterson (1967Peterson ( , 1969 and MacQueen (1968), independently, detected a sharp peak in the near-infrared brightness of the solar corona at 4 R from the Sun during the total solar eclipse of 1966. Because the near-infrared peak appeared simultaneously at the east and the west side of the Sun, Peterson (1967Peterson ( , 1969 concluded that the near-solar dust grains move in circular orbit. Based on a balloon-borne observation of the 1983 eclipse, Mizutani et al (1984) have suggested the concentration of the near-solar dust cloud towards the ecliptic plane in order to explain a detected feature in the east-west side slope of the brightness.…”

Section: The Configuration Of the Dust Cloud Near The Sunsupporting

confidence: 70%

“…The effect of the dust-free zone on thermal emission brightness has been supposed to cause the sharp break of the brightness at the edge of the dust-free zone (Peterson, 1963). As might have been expected, Peterson (1967Peterson ( , 1969 and MacQueen (1968), independently, detected a sharp peak in the near-infrared brightness of the solar corona at 4 R from the Sun during the total solar eclipse of 1966. Because the near-infrared peak appeared simultaneously at the east and the west side of the Sun, Peterson (1967Peterson ( , 1969 concluded that the near-solar dust grains move in circular orbit.…”

Section: The Configuration Of the Dust Cloud Near The Sunmentioning

confidence: 79%

“…H-band: Peterson (1971); Mizutani et al (1984); Maihara et al (1985); Lamy et al (1992); Kuhn et al (1994); Tollestrup et al (1994). K-band: Peterson (1967Peterson ( , 1969Peterson ( , 1971MacQueen (1968); Adney (1973); Strong (1974); Rao et al (1981); Mampaso et al (1982Mampaso et al ( , 1983; Mizutani et al (1984); Maihara et al (1985); Hodapp et al (1992); Lamy et al (1992); Skomorovsky et al (1992); Kuhn et al (1994);MacQueen et al (1994). L'-band: Mizutani et al (1984); Maihara et al (1985).…”

Section: Disappearance Of the Excess Emission In The Near-infrared Brmentioning

confidence: 99%

“…In addition, high eccentricity of the sungrazing comets prevents the cometary dust from staying in a bound orbit around the Sun and the supply of cometary dust from the sungrazer is a very local phenomenon that is inconsistent with the symmetrical feature of the near-infrared hump around 4 R on the both side of the Sun (cf. Peterson, 1967Peterson, , 1969. Although the cometary dust grains temporarily increase the coronal brightness (Michels et al, 1982), the observable time is too short to explain the excess emission of near-infrared brightness detected over several months (cf.…”

Section: Disappearance Of the Excess Emission In The Near-infrared Brmentioning

confidence: 99%

“…Since the sixties, further information has been obtained from nearinfrared observations (Peterson, 1967(Peterson, , 1969MacQueen, 1968), and with infrared imaging systems in the nineties (Hodapp et al, 1992;Kuhn et al, 1994;Tollestrup et al, 1994).…”

Section: Introductionmentioning

confidence: 99%

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Brightness of the solar F-corona

Kimura

Mann

2014

Earth Planet Sp

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We discuss our present knowledge about the brightness of the solar F-corona in the wavelength range from the visible to the middle infrared. From the general trend of the observational data, the F-corona is regarded as the continuous extension of the zodiacal light at smaller elongation of the line of sight. A contribution of thermal emission from dust is indicated by the increasing F-coronal brightness in comparison to the solar spectrum towards longer wavelength. As compared with the F-coronal brightness, the polarization and color in the visible regime are not well determined due to the high sensitivity of these quantities to the observational accuracy. Aside from observational problems, our present interpretation of the F-coronal brightness is also limited due to ambiguities in the inversion of the line of sight integral. Nevertheless, the measurements and model calculations of the brightness can be used to deduce some physical properties of dust grains. We show that the hump of the near-infrared brightness at 4 solar radii, which was sometimes observed in the corona, is related rather to the physical properties of dust grains along the line of sight than to the existence of a dust ring as previously discussed. We also show that the appearance or disappearance of the near-infrared peak in the coronal brightness cannot be described in any periodic cycle for each wavelength range.

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