Comet Publications Used in Preparing the 2005 Triennial Report

       

The ADS abstract service (http://adsabs.harvard.edu/abstract_service.html) was searched for papers appearing in refereed publications during the period between July 2002 and June 2005, inclusive, on the term "COMET". This returned 917 abstracts plus 37 papers published in the Comet II book that are not considered to be refereed papers by the ADS.

 

From these 954 papers, 361 were selected as falling under the purview of the Physical Studies of Comets Working Group. That is, no papers on purely meteoritic, interplanetary dust (including cometary trails), dynamical, or astrometric studies were included. Papers presenting ground-based instrumentation or space instrumentation or missions for future comet studies were not taken into consideration either. However, papers presenting laboratory experiments for the understanding of the origin of cometary material were included.

 

The 361 relevant papers were sorted into nine categories and a brief description of the scientific results in each category was written citing a subset of them. The titles and abstracts for the entire list of 361 papers appear below. The order of this list is that returned by the ADS search engine, i.e., it is not in alphabetical or chronological order. A paper cited in the IAU Triennial Report can be located using the browser or PDF reader’s “Find” function.

 

This list was prepared by D. Bockelée-Morvan on 20 September 2005

 


Title:

 

On the ejection velocity of meteoroids from comets

Authors:

 

Ma, Yuehua; Williams, I. P.; Chen, Wenping

Affiliation:

 

AA(Purple Mountain Observatory, Academia Sinica, Nanjing 210008, China; and National Astronomical Observatories, Academia Sinica, China; ), AB(Astronomy Unit, Queen Mary, University of London, London E1 4NS), AC(Institute of Astronomy, National Central University, Taiwan 32054)

Journal:

 

Monthly Notice of the Royal Astronomical Society, Volume 337, Issue 3, pp. 1081-1086. (MNRAS Homepage)

Publication Date:

 

12/2002

Origin:

 

MNRAS

MNRAS Keywords:

 

comets: general, meteors, meteoroids

Abstract Copyright:

 

(c) RAS

DOI:

 

10.1046/j.1365-8711.2002.05996.x

Bibliographic Code:

 

2002MNRAS.337.1081M

Abstract

The ejection of meteoroids from comets has been discussed by many authors and is a problem that is important both for a full understanding of cometary processes and for the evolution of meteoroid streams. We reinvestigate the problem here, starting from simple physical principles, and compare the results that we obtain with those of other authors, in particular Whipple.


 

Title:

 

Erratum: On the source of C(1D) atoms in cometary comae

Authors:

 

Saxena, P. P.; Bhatnagar, S.; Singh, M.

Journal:

 

Monthly Notice of the Royal Astronomical Society, Volume 337, Issue 2, pp. 768-768. (MNRAS Homepage)

Publication Date:

 

12/2002

Origin:

 

MNRAS

MNRAS Keywords:

 

errata, addenda, molecular processes, comets: individual: Comet Halley, comets: individual: Comet West, comets: individual: Comet Bradfield (1979 X)

Abstract Copyright:

 

(c) RAS

DOI:

 

10.1046/j.1365-8711.2002.06092.x

Bibliographic Code:

 

2002MNRAS.337..768S

Abstract

Not Available


 

Title:

 

X-Ray Emission from Comet McNaught-Hartley (C/1999 T1)

Authors:

 

Krasnopolsky, V. A.; Christian, D. J.; Kharchenko, V.; Dalgarno, A.; Wolk, S. J.; Lisse, C. M.; Stern, S. A.

Journal:

 

Icarus, Volume 160, Issue 2, p. 437-447. (Icarus Homepage)

Publication Date:

 

12/2002

Origin:

 

ELSEVIER

Abstract Copyright:

 

(c) 2002 Elsevier Science (USA)

DOI:

 

10.1006/icar.2002.6965

Bibliographic Code:

 

2002Icar..160..437K

Abstract

Comet McNaught-Hartley was observed in five 1-h exposures on January 8-14 2001 using the advanced CCD imaging spectrometer on board the Chandra X-ray Observatory. The X-ray image of the comet does not show a crescent-like shape. The brightest region is offset from the nucleus between the sunward and comet velocity directions. The comet mean X-ray luminosity is equal to 7.8×1015 erg s-1 for photon energy E>150 eV and aperture ρ=1.5×105 km where the comet X-ray brightness exceeds 20% of the peak value. Gas production rate was 1029 s-1 during the observations, and the efficiency of X-ray excitation was equal to 4×10-14 erg AU3/2. Day-to-day variations in X-rays reached a factor of 5. The strongest short-term variation was by a factor of 1.75 for 1600 s. This variation may be explained by a decline in the solar-wind flux by the same factor in ~800 s. The comet and Earth were seeing different faces of the Sun, and time delay in the solar-wind events on the Earth and the comet was long, equal to 6 days. The best correlation between the comet X-ray luminosity and the solar-wind proton density is for the time delay of 5.5 days and may be explained by the higher velocity of heavy ions. Careful background subtraction made it possible to extract the comet spectrum from 150 to 1000 eV. No signal was detected at E>1000 eV, and a 3σ upper limit to any emission with E>1000 eV is 0.3% of the photon emission at 150-1000 eV. The best χ2-fit model to the spectrum consists of nine narrow emission features. The emission energies and intensities are in good agreement with a charge exchange spectrum calculated by us for the slow solar wind. Using this spectrum, we identify the observed emissions as (Ne7++Mg7++Mg8+) at 195 eV, (Mg8++Mg9++Si8+) at 250 eV, C5+ at 370 and 460 eV, O6+ at 560 eV, O7+ at 650, 780, and 840 eV, and Ne8+ at 940 eV. X-ray spectroscopy of comets may be used to diagnose the solar-wind composition and its interaction with comets.


 

Title:

 

The Dust in Comet C/1999 S4 (LINEAR) during Its Disintegration: Narrow-Band Images, Color Maps, and Dynamical Models

Authors:

 

Bonev, T.; Jockers, K.; Petrova, E.; Delva, M.; Borisov, G.; Ivanova, A.

Affiliation:

 

AA(Institute of Astronomy, 72 Tsarigradsko chaussée Boulevard, Sofia, 1784 Bulgaria), AB(Max-Planck-Institut für Aeronomie, Katlenburg-Lindau, 37191, Germany), AC(Space Research Institute, Moscow Russia), AD(Institut für Weltraumforschung, Graz Austria), AE(Institute of Astronomy, 72 Tsarigradsko chaussée Boulevard, Sofia, 1784 Bulgaria), AF(Institute of Astronomy, 72 Tsarigradsko chaussée Boulevard, Sofia, 1784 Bulgaria)

Journal:

 

Icarus, Volume 160, Issue 2, p. 419-436. (Icarus Homepage)

Publication Date:

 

12/2002

Origin:

 

ELSEVIER

Abstract Copyright:

 

(c) 2002 Elsevier Science (USA)

DOI:

 

10.1006/icar.2002.6971

Bibliographic Code:

 

2002Icar..160..419B

Abstract

Comet C/1999 S4 was observed with the 2m-telescopes of the Bulgarian National Observatory and Pik Terskol Observatory, Northern Caucasus, Russia, at the time of its disintegration. Maps of the dust brightness and color were constructed from images obtained in red and blue continuum windows, free from cometary molecular emissions. We analyze the dust environment of Comet C/1999 S4 (LINEAR) taking into account the observed changes apparent in the brightness images and in plots of Afρ profiles as function of the projected distance ρ from the nucleus. We also make use of the syndyne-synchrone formalism and of a Monte Carlo model based on the Finson-Probstein theory of dusty comets. The brightness and color of individual dust particles, which is needed to derive theoretical brightness and color maps of the cometary dust coma from the Monte Carlo model, is determined from calculations of the light scattering properties of randomly oriented oblate spheroids. In general, the dust of Comet C/1999 S4 (LINEAR) is strongly reddened, with reddening values up to 30%/1000 Å in some locations. Often the reddening is higher in envelopes further away from the nucleus. We observed two outbursts of the comet with brightness peaks on July 14 and just before July 24, 2000, when the final disintegration of the comet started. During both outbursts an excess of small particles was released. Shortly after both outbursts the dust coma ``turns blue.'' After the first outburst, the whole coma was affected; after the second one only a narrow band of reduced color close to the tail axis was formed. This difference is explained by different terminal ejection speeds, which were much lower than normal in case of the second outburst. In particular in the second, final outburst the excess small particles could originate from fragmentation of ``fresh'' larger particles.


 

Title:

 

A McDonald Observatory Study of Comet 19P/Borrelly: Placing the Deep Space 1 Observations into a Broader Context

Authors:

 

Farnham, Tony L.; Cochran, Anita L.

Journal:

 

Icarus, Volume 160, Issue 2, p. 398-418. (Icarus Homepage)

Publication Date:

 

12/2002

Origin:

 

ELSEVIER

Abstract Copyright:

 

(c) 2002 Elsevier Science (USA)

DOI:

 

10.1006/icar.2002.6969

Bibliographic Code:

 

2002Icar..160..398F

Abstract

We present imaging and spectroscopic data on Comet 19P/Borrelly that were obtained around the time of the Deep Space 1 encounter and in subsequent months. In the four months after perihelion, the comet showed a strong primary (sunward) jet that is aligned with the nucleus' spin axis. A weaker secondary jet on the opposite hemisphere appeared to become active around the end of 2001, when the primary jet was shutting down. We investigated the gas and dust distributions in the coma, which exhibited strong asymmetries in the sunward/antisunward direction. A comparison of the CN and C2 distributions from 2001 and 1994 (during times when the viewing geometry was almost identical) shows that each species is remarkably similar, indicating that the comet's activity is essentially repeatable from one apparition to the next. We also measured the dust reflectivities as a function of wavelength and position in the coma, and though the dust was very red overall, we again found variations with respect to the solar direction. We used the primary jet's appearance on several dates to determine the orientation of the rotation pole to be α=214°, δ=-5°. We compared this result to published images from 1994 to conclude that the nucleus is near a state of simple rotation. However, data from the 1911, 1918, and 1925 apparitions indicate that the pole might have shifted by 5-10° since the comet was discovered. Using our pole position and the published nongravitational acceleration terms, we computed a mass of the nucleus of 3.3×1016 g and a bulk density of 0.49 g cm-3 (with a range of 0.29<ρ<0.83 g cm-3). This result is the least model-dependent comet density known to date.


 

Title:

 

Long-Term Evolution of Objects in the Kuiper Belt Zone-Effects of Insolation and Radiogenic Heating

Authors:

 

Choi, Young-Jun; Cohen, Merav; Merk, Rainer; Prialnik, Dina

Affiliation:

 

AA(Department of Geophysics and Planetary Sciences, Tel Aviv University, Ramat Aviv, 69978 Israel), AB(Department of Geophysics and Planetary Sciences, Tel Aviv University, Ramat Aviv, 69978 Israel), AC(Department of Geophysics and Planetary Sciences, Tel Aviv University, Ramat Aviv, 69978 Israel), AD(Department of Geophysics and Planetary Sciences, Tel Aviv University, Ramat Aviv, 69978, Israel)

Journal:

 

Icarus, Volume 160, Issue 2, p. 300-312. (Icarus Homepage)

Publication Date:

 

12/2002

Origin:

 

ELSEVIER

Abstract Copyright:

 

(c) 2002 Elsevier Science (USA)

DOI:

 

10.1006/icar.2002.6976

Bibliographic Code:

 

2002Icar..160..300C

Abstract

The Kuiper Belt zone is unique insofar as the major heat sources of objects a few tens of kilometers in size-solar radiation on the one hand and radioactive decay on the other-have comparable power. This leads to unique evolutionary patterns, with heat waves propagating inward from the irradiated surface and outward from the radioactively heated interior. A major radioactive source that is considered in this study is 26Al. The long-term evolution of several models with characteristics typical of Kuiper Belt objects is followed by means of a 1-D numerical code that solves the heat and mass balance equations on a spherically symmetric grid. The free parameters considered are radius (10-500 km), heliocentric distance (30-120 AU), and initial 26Al content (0-5×10-8 by mass). The initial composition assumed is a porous mixture of ices (H2O, CO, and CO2) and dust. Gases released in the interior are allowed to escape to the surface. It is shown that, depending on parameters, the interior may reach quite high temperatures (up to 180 K). The models suggest that Kuiper Belt objects are likely to lose the ices of very volatile species during early evolution; ices of less volatile species are retained in a surface layer, about 1 km thick. The models indicate that the amorphous ice crystallizes in the interior, and hence some objects may also lose part of the volatiles trapped in amorphous ice. Generally, the outer layers are far less affected than the inner part, resulting in a stratified composition and altered porosity distribution. These changes in structure and composition should have significant consequences for the short-period comets, which are believed to be descendants of Kuiper Belt objects.


 

Title:

 

Spectrophotometry of the comets C/2000 WM1 (LINEAR) and C/2002 C1 (IkeyaZhang)

Authors:

 

Sanwal, B. B.; Kumar, Brijesh; Singh, Mahendra

Affiliation:

 

AA(State Observatory, Manora Peak, Nainital 263129, India), AB(State Observatory, Manora Peak, Nainital 263129, India), AC(State Observatory, Manora Peak, Nainital 263129, India)

Journal:

 

Bulletin of the Astronomical Society of India, vol. 30, p.943-950 (BASI Homepage)

Publication Date:

 

12/2002

Origin:

 

BASI

Keywords:

 

Comet spectrophotometry, column densities and production rates

Bibliographic Code:

 

2002BASI...30..943S

Abstract

Spectrophotometric observations of the coma of the comets C/2000 WM1 (LINEAR) and C/ 2002 C1 (Ikeya-Zhang) were taken during Nov, Dec 2001 and Mar, Apr 2002 respectively with 104-cm telescope of the State Observatory, Nainital. CN (3883) and C2 swan bands (4695, 5165 and 5538) have been identified in both the comets. Na I emission was detected in comet Ikeya-Zhang. An estimate of CN and C2 abundances and their production rates have been derived. Dust production rates have also been determined.


 

Title:

 

Fragmentation Origin of Major Sungrazing Comets C/1970 K1, C/1880 C1, and C/1843 D1

Authors:

 

Sekanina, Zdenek; Chodas, Paul W.

Affiliation:

 

AA(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109; zs@sek.jpl.nasa.gov, ), AB(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109; zs@sek.jpl.nasa.gov, )

Journal:

 

The Astrophysical Journal, Volume 581, Issue 2, pp. 1389-1398. (ApJ Homepage)

Publication Date:

 

12/2002

Origin:

 

UCP

ApJ Keywords:

 

Comets: General, Comets: Individual: Alphanumeric: X/1106 C1, comets: individual (C/1843 D1, C/1880 C1), Comets: Individual: Alphanumeric: C/1882 R1, Comets: Individual: Alphanumeric: C/1887 B1, Comets: Individual: Alphanumeric: C/1945 X1, Comets: Individual: Alphanumeric: C/1963 R1, Comets: Individual: Alphanumeric: C/1965 S1, Comets: Individual: Alphanumeric: C/1970 K1, Comets: Individual: Alphanumeric: D/1993 F2, Methods: Data Analysis

Abstract Copyright:

 

(c) 2002: The American Astronomical Society

DOI:

 

10.1086/344261

Bibliographic Code:

 

2002ApJ...581.1389S

Abstract

Following our recent successful modeling of the common origin of two of the brightest members of the Kreutz system of sungrazing comets, we now examine three other objects: C/1970 K1 (White-Ortiz-Bolelli), the most recent sungrazer discovered from Earth, C/1880 C1 (Great Southern Comet), and C/1843 D1 (Great March Comet). For White-Ortiz-Bolelli, five possible origin and orbit evolution scenarios are explored. We find that its parent was neither C/1965 S1 (Ikeya-Seki), nor C/1882 R1 (Great September Comet), nor the comet of 1106 (the presumed parent of Ikeya-Seki and the 1882 comet). The motion of C/1970 K1 is consistent with a scenario in which the parent was an unknown fragment that separated from the 1106 comet at the same time as, or shortly before, Ikeya-Seki and passed through perihelion in 1970 June-July, shortly after White-Ortiz-Bolelli. The separation of White-Ortiz-Bolelli from this fragment is found to have occurred around the mid-eighteenth century, at a heliocentric distance of about 150 AU, with a relative velocity of 3-5 m s-1 in the general direction of the Sun and to the north of the orbital plane. On the other hand, we conclude that the 1880 comet separated directly from C/1843 D1, the second brightest known sungrazer, some 100-150 days after the 1843 comet's previous perihelion passage in the eleventh century, at 2.5-3 AU from the Sun, with a relative velocity of slightly more than 7 m s-1 in the generally antisolar direction and to the south of the orbital plane. The pattern of fragmentation of the Kreutz system's members discovered from Earth begins to resemble the evolution of the system's minor fragments detected coronagraphically from aboard the SOHO spacecraft, and there is significant qualitative similarity with fragmentation of comet D/1993 F2 (Shoemaker-Levy 9).


 

Title:

 

Measurements of [C I] Emission from Comet Hale-Bopp

Authors:

 

Oliversen, R. J.; Doane, N.; Scherb, F.; Harris, W. M.; Morgenthaler, J. P.

Affiliation:

 

AA(NASA Goddard Space Flight Center, Greenbelt, MD 20771; ron@midnight.gsfc.nasa.gov.; Visiting Astronomer at the National Solar Observatory, operated by the Association for Research in Astronomy, under contract to the National Science Foundation.), AB(Visiting Astronomer at the National Solar Observatory, operated by the Association for Research in Astronomy, under contract to the National Science Foundation.; NASA Goddard Space Flight Center, Greenbelt, MD 20771.; Currently at Department of Astronomy, University of Wisconsin, Madison, WI 53706; doane@astro.wisc.edu.), AC(Visiting Astronomer at the National Solar Observatory, operated by the Association for Research in Astronomy, under contract to the National Science Foundation.; Department of Physics, University of Wisconsin, Madison, WI 53706; scherb@physics.wisc.edu, jpmorgen@alum.mit.edu.), AD(Space Astronomy Lab, University of Wisconsin, Madison, WI 53706; wharris@sal.wisc.edu.), AE(Department of Physics, University of Wisconsin, Madison, WI 53706; scherb@physics.wisc.edu, jpmorgen@alum.mit.edu.)

Journal:

 

The Astrophysical Journal, Volume 581, Issue 1, pp. 770-775. (ApJ Homepage)

Publication Date:

 

12/2002

Origin:

 

UCP

ApJ Keywords:

 

Comets: Individual: Name: Hale-Bopp (C/1995 O1)

Abstract Copyright:

 

(c) 2002: The American Astronomical Society

DOI:

 

10.1086/344149

Bibliographic Code:

 

2002ApJ...581..770O

Abstract

We present quantitative measurements of cometary [C I] 9850 Å emission obtained during observations of comet Hale-Bopp (C/1995 O1) in 1997 March and April. The observations were carried out using a high-resolution (λ/Δλ~40,000) Fabry-Pérot/CCD spectrometer at the McMath-Pierce Solar telescope on Kitt Peak. This forbidden line, the carbon analog of [O I] 6300 Å, is emitted in the radiative decay of C(1D) atoms. In the absence of other sources and sinks, [C I] 9850 Å emission can be used as a direct tracer of CO photodissociation in comets. However, in Hale-Bopp's large, dense coma, other processes, such as collisional excitation of ground-state C(3P), dissociative recombination of CO+, and collisional dissociation of CO and CO2 may produce significant amounts of C(1D). The long C(1D) radiative lifetime (~4000 s) makes collisional deexcitation (quenching) the primary loss mechanism in the inner coma. Thus, a detailed, self-consistent global model of collisional and photochemical interactions is necessary to fully account for [C I] 9850 Å emission in comet Hale-Bopp.


 

Title:

 

Common Origin of Two Major Sungrazing Comets

Authors:

 

Sekanina, Zdenek; Chodas, Paul W.

Affiliation:

 

AA(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109; zs@sek.jpl.nasa.gov, ), AB(Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109; zs@sek.jpl.nasa.gov, )

Journal:

 

The Astrophysical Journal, Volume 581, Issue 1, pp. 760-769. (ApJ Homepage)

Publication Date:

 

12/2002

Origin:

 

UCP

ApJ Keywords:

 

Celestial Mechanics, Comets: General, Comets: Individual: Alphanumeric: X/1106 C1, comets: individual (C/1882 R1, C/1965 S1), Comets: Individual: Alphanumeric: D/1993 F2, Methods: Numerical

Abstract Copyright:

 

(c) 2002: The American Astronomical Society

DOI:

 

10.1086/344216

Bibliographic Code:

 

2002ApJ...581..760S

Abstract

Our extensive orbital calculations show that the motion of comet C/1965 S1 (Ikeya-Seki), a major member of the Kreutz sungrazing system, can be derived from the motion of its ``sister'' comet C/1882 R1 (Great September Comet) on the assumption that the two objects are fragments of a common parent that split in the year 1106, at the time when a very bright comet appeared near the Sun according to a number of historical records. Specifically, the orbit of Ikeya-Seki derived from astrometric positions in 1965-1966 is matched with remarkably high accuracy, well within the errors of observation, by (1) integrating the motion of comet C/1882 R1 back to 1106; (2) launching from the parent a fragment some 18 days after perihelion, 0.75 AU from the Sun, with a relative velocity of about 7 m s-1 nearly in the antisolar direction; and (3) integrating the fragment's motion forward to 1965. We find that having the break-up closer to the Sun or before perihelion yields grossly inferior solutions. We conclude that the fragmentation event itself was not tidal in nature, but appears to have been due to rotational, and possibly other, forces acting on the parent comet, afflicted with cracks and fissures caused by the Sun's tidal forces a few weeks earlier. We note that the derived separation velocity is in the range established for nontidal fragmentation of minor sungrazers at large heliocentric distances and that there are obvious similarities with the behavior of comet D/1993 F2 (Shoemaker-Levy 9) following its close encounter with Jupiter in 1992 July.


 

Title:

 

The Origin of the Solar Wind

Authors:

 

Woo, Richard; Habbal, Shadia Rifai

Journal:

 

American Scientist, vol. 90, Issue 6, p.532

Publication Date:

 

12/2002

Origin:

 

WEB

Bibliographic Code:

 

2002AmSci..90..532W

Abstract

Nearly 1,400 years ago, Chinese astronomers noticed that comet tails always point away from the Sun. They concluded that the Sun must have <em>chi</em>—a basic life force—that blows the tails away. It wasn't until the middle of the 20th century that scientists understood that this "force" actually consisted of little pieces of the sun itself—protons and electrons—blowing out into the solar system as a "wind" at