IUE observations of comet P/Halley: evolution of the ultraviolet spectrum between September 1985 and July 1986

Feldman, P. D.; Festou, M. C.; A’Hearn, M. F.; Arpigny, C.; Butterworth, P. S.; Cosmovici, C. B.; Danks, A. C.; Gilmozzi, R.; Jackson, William M.; McFadden, L. A.; Patriarchi, P.; Schleicher, D. G.; Tozzi, G. P.; Wallis, M. K.; Weaver, Harold A.; Woods, Thomas N.

doi:10.1007/978-3-642-82971-0_59

Cited by 21 publications

(15 citation statements)

References 12 publications

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“…However, observations of OH are difficult because the (0, 0) band of OH is at 3080Å where atmospheric transmission is low. Observations of OH are best done with a UV telescope such as IUE or HST (e.g., Weaver et al 1981, Feldman et al 1987, but OH can be detected with some ground-based instruments (e.g., Cochran andSchleicher 1993, A'Hearn et al 1995). Radio observations can also be used to study OH and are excellent for velocity resolution but generally are lacking in spatial resolution because of the very long wavelength and, hence, large beam size (e.g., Bockelée-Morvan et al 1990, Crovisier 1989, Gérard 1990).…”

Section: Resultsmentioning

confidence: 99%

Observations of O (1S) and O (1D) in Spectra of C/1999 S4 (LINEAR)

Cochran

2001

Icarus

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Section: Resultsmentioning

confidence: 99%

Observations of O (1S) and O (1D) in Spectra of C/1999 S4 (LINEAR)

Cochran

2001

Icarus

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“…The flybys of the three spacecraft discussed in the current paper is covered by the period over which the activity of the comet was monitored, shown in Fig. 8 of Feldman et al (1987). It was found that the water production had a strong decrease from ∼ 1.5 × 10 30 to ∼ 5.0 × 10 29 molecules s −1 on 7 March.…”

Section: Cometary Outgassingmentioning

confidence: 94%

“…Tátrallyay et al (2000a) investigated the VEGA 1 and 2 plasma data and found that the density of the plasma flow for the VEGA 1 encounter was much higher than for the VEGA 2 encounter. Gehrz et al (2005) used the Lyα measurement from the Pioneer Venus UV spectrometer (Stewart, 1987) and the OH measurements from the IUE (Feldman et al, 1987) of comet 1P/Halley to obtain the water production rate. The flybys of the three spacecraft discussed in the current paper is covered by the period over which the activity of the comet was monitored, shown in Fig.…”

Section: Cometary Outgassingmentioning

confidence: 99%

A comparison between VEGA 1, 2 and Giotto flybys of comet 1P/Halley: implications for Rosetta

et al. 2014

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Abstract. Three flybys of comet 1P/Halley, by VEGA 1, 2 and Giotto, are investigated with respect to the occurrence of mirror mode waves in the cometosheath and field line draping in the magnetic pile-up region around the nucleus. The time interval covered by these flybys is approximately 8 days, which is also the approximate length of an orbit or flyby of Rosetta around comet 67P/Churyumov-Gerasimenko. Thus any significant changes observed around Halley are changes that might occur for Rosetta during one pass of 67P/CG. It is found that the occurrence of mirror mode waves in the cometosheath is strongly influenced by the dynamical pressure of the solar wind and the outgassing rate of the comet. Field line draping happens in the magnetic pile-up region. Changes in nested draping regions (i.e. regions with different B x directions) can occur within a few days, possibly influenced by changes in the outgassing rate of the comet and thereby the conductivity of the cometary ionosphere.

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“…Observations of CS in Comet IRAS-Araki-Alcock (1983 VII) by the IUE satellite have demonstrated that the short-lived (scale length « 300 km) parent of CS (scale length « 100,000 km) is the molecule CS 2 ). The IUE satellite monitored the CS production rate in Halley (Feldman et al 1987). A uniform decrease in the production rate toward larger heliocentric distances was found.…”

Section: Sulfur and Hydrocarbonsmentioning

confidence: 98%

“…The H2O gas production rates as a function of the heliocentric distance of Halley were retrieved from the fluorescent emission of OH (0-0 band) from IUE data , Feldman et al 1986b. Pre-and post-perihelion observations of the OH emission are also available from the Soviet ASTRON satellite (Boyarchuk et al 1987).…”

Section: Water Vapormentioning

confidence: 99%

The Composition of Comets

Krankowsky

1991

International Astronomical Union Colloquium

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ABSTRACT. The chemical composition of gases in the coma of Comet Halley obtained from in situ and remote observations is reviewed. Water vapor with an abundance of approximately 80% by number is the dominant parent gas. Carbon monoxide is the second most abundant molecule, with about one-seventh of the water abundance. The other expected parent gasescarbon dioxide, methane, and ammonia-contributed with at most a few percent to the coma gas. Molecular nitrogen is found to be a minor species, with an abundance of less than one percent. Formaldehyde is relatively abundant, with a few percent relative to water. Gas-phase isotope ratios of nitrogen, oxygen, and sulfur are found to agree with solar system values within experimental errors. Halley's hydrogen isotope ratio is comparable t o t h e values found in other solar system objects poor in hydrogen, but distinctly different from t h e protosolar nebula and objects that accreted hydrogen in gaseous form. Carbon in the cyanide radical is enriched by 35% in 1 3 C compared to the bulk solar system value that indicates the presence of non-homogenized interstellar carbon in Halley. Volatiles released from grains contribute noticeably to the coma gas. Complex organic molecules, inferred from various observations as constituents of the dust grains, are believed to be the origin of the distributed C O source, CN, and other jet structures in the coma.

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IUE observations of comet P/Halley: evolution of the ultraviolet spectrum between September 1985 and July 1986

Cited by 21 publications

References 12 publications

Observations of O (1S) and O (1D) in Spectra of C/1999 S4 (LINEAR)

Observations of O (1S) and O (1D) in Spectra of C/1999 S4 (LINEAR)

A comparison between VEGA 1, 2 and Giotto flybys of comet 1P/Halley: implications for Rosetta

The Composition of Comets

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