From the brightness development and a sequence of imaging observations of the coma activity onset of comet P/Tempel 2 in 1988, it is concluded that there might have happened eruptive events of strong dust and gas outbursts during May and June 1988. A comparison of dust coma modeling calculations with CCD observations of the coma widely confirms Sekanina's nucleus model for the comet

Baer, A.

Boehnhardt, Hermann

Massonne, L.

English

NASA Technical Reports Server

Asteroids, Comets, Meteors 1991, pp. 77-80
Lunar and Planetarylnstitute, Houston, ,992 __ /_ 77N i30
COMET P/Tgl_EL - 501_ HIGHLIGHTS AND CONCLUSIONS
FROM THE 1988 APPARITION *
H. 8oehnhardt, (Dr.-Remeis Sternwarte, Bamberg, and
mbp Software & Systems, Dortmund)
A. 8_r, (Dr.-Remeis Sternwarte, 8amberg)
L. Massonne (mbp Software & Systems, Dortmund)
* based in part on observations obtained at the European
Southern Observatory ESO, La Silla/Chile.
Abstract: From the brightness development and a sequence of
imaging observations of the coma activity onset of comet
P/Tempel 2 in 1988, it is concluded that there might have
happened eruptive events of strong dust and gas outburts during
May and June 1988. A comparison of dust coma modelling
calculations with CCD observations of the coma widely confirms
Sekanina's nucleus model for the comet.
1. Introduction
During the 1988 apparition of comet P/Tempel 2 a series of
observations were performed by a team of the Bamberg observatory
and some external collaborators (in total II team members}. The
team work was supplemented by amateur observers who contributed
the visual brightness estimations of the comet. The scientific
aims of the observations were to estimate the nucleus size, to
monitor the coma activity and its morphology, to derive some
characteristic values of the gas productions of C2, C3 and CN
together with basic data on molecular physics of C2 and to
provide position measurements for an improved orbit
determination of the comet. The results of this research project
on P/Tempel 2 (except the astrometry} are published in
Boehnhardt et al. (199%}.
In this paper we present some further conclusions on possible
eruptive events during the preperihelion activity phase of
P/Tempel 2 and a comparison of the coma imaging observations
with dust coma model calculations of the comet.
2. Eruptive events in the lightcurve and the coma development
From the published imaging and photometry of comet P/Tempel 2
during the transition phase of marginal to significant coma
activity (see Jewitt and Luu, 199%: 9-15/4/88 = probably no
coma; Boehnhardt et al., 1996: 4/5/88 = no coma; Wisniswski,
199%: 8-9/5/88 = faint coma; West, 1988: 17/5/88 = significant
coma} we conclude that the onset of major gas and dust
production of the cometary nucleus took place between 135 to 131
days before perihelion, i.e. at the rather close solar distance
https://ntrs.nasa.gov/search.jsp?R=19930009941 2020-03-17T07:34:27+00:00Z
78 Asteroids, Comets, Meteors 1991
of 1.9 AU. At similar solar distances most comets have already
developed prominent comae. At the same time interval
preperihelion the visual lightcurve of the comet showed an
instantaneous increase of about 3 magnitudes (from 16.5 nag
nuclear to 13.5 mag coma brightness; see Weiss, 19895. The
temporal coincidence of both phenomena could have been caused by
an eruptive onset of gas and dust emission from a large and
highly active surface area of the nucleus. The weak gas emission
of P/Tempel 2 observed by Cochran (19915 from February 1988
onwards may therefore resemble either the moderate outgassing of
the inactive surface of the nucleus or it may indicate the
eventual "smoke" of the activity centre of the May eruption.
Before early May 1988 this active region seemed to have been
protected against sunlight (either by a surface crust or by
shadowing effects due to surface geometry}. After the activity
onset in May 1988 the cometary brightness remained constant for
about 58 days. Thereafter, a second rapid brightness increase
can be seen in the reported lightcurve (Boehnhardt et al.,
199e}. A similar behaviour of P/Tempel 2 i.e. a brightness
plateau with a successive eruptive brightness increase, can also
be inferred from the 1967 lightcurve of the comet (Weiss, 19895.
It would be interesting to look for similar features of eruptive
events and for their temporal repetition or non-repetition
during the forthcoming apparitions of P/Tempel 2.
3. Coma morphology - observations and mode!linq
Figs. l-3a show V-filter CCD exposures of comet P/Tempel 2
obtained on 17/5/88 (West, 1988), on 24/7/88 (Boehnhardt et al.,
199%} and on 7/11/88 (Richtler, 1989, so far unpublished5,
respectively. All images exhibit a prominent fan-shaped coma,
which can basically be interpreted as due to a jet of dust and
gas emitted from a very active region located at h_gh
cometographic latitude. Since the V-filter transmission is
dominated by reflected sunlight from the cometary dust, we
assume that the coma images widely resemble the dust
distribution as seen from Earth. The jet was smeared by the
rotation of the nucleus which finally resulted in the fan-shaped
coma of the comet. Sekanina (1979, 1987) has proposed a nucleus
model for P/Tempel 2 which claimes an activity centre at about
6% deg cometographic latitude as source for the coma fan. This
centre rotates in about 9 hours (Jewitt and Luu, 1989) about the
rotation axis at right ascension 147 deg and declination +55 deg
(epoch 195%5. The nucleus was found to be of size 16 x 8 x 8 km
(see for instance Sekanina, 1988}. According to Sekanina (1987}
the fan axis observed should roughly indicate the direction of
the projected rotation axis. In order to assess the fan axis
more accurately the observations on 24/7/88 and 7/11/88 were
computer-processed by the so called radial renormalisation
method: this method reduces the general coma background and
enhances faint inherent coma structures. It is comparable to the
method successfully applied by A'Hearn et al. (1986} for the CN
Asteroids, Comets, Meteors 1991 79
Fiqure I to 3
1
a
b
2
a
b
c
3
a
b
c
P/Tempel 2 - a comparison of observed (a),
calculated (b) and renormalized (c) cola flages
North is up and East to the right, the Sun is
indicated by o, the direction of the projected
rotation axis of the nucleus by an arrow.
PITempel 2 on 1988105117 (from West, 1988)
CCD image (42000 km x 42000 km)
computer simulation (25000 km x 25000 kl)
PITempel 2 on 1988107124
CCD image (30000 kn x 38000 Eu)
computer simulation (190000 km x 190000 km)
renormalized coma image (17000 km x 17000 km)
PITempel 2 on 1988111107
CCD image (60000 km x 60000 km)
computer simulation (200000 km x 200000 kn)
renormalized coma image (58000 km x 58000 _)
]b
2a
38
2b
It
3b
0
0
2C
3C
80 Asteroids, Comets, Meteors 1991
jets in comet P/Halley. For both observing dates the alignment
of the fan axis with the predicted direction of the projected
rotation axis is rather good (see figs. 2c, 3c). However, for
the observation on 17/5/88 a significant discrepancy between fan
axis and projected rotation axis can be found (see fig. la}.
In order to check Sekanina's model for P/Tempel 2 more
thoroughly computer simulations were performed using the ESOC
dust coma modelling software. The physical principles and the
computer programs of the software package are described in
Massonne (1986). The results of this computer simulations for
the dust coma of P/Tempel 2 are presented in figs 1-3b. The
figures show the dust density distribution as seen from Earth
for the three observation dates from above. Though in the
present software version some simplified assumptions are made
(spherical nucleus, fixed rotation axis, dust size distribution
of P/Halley), the modelling verifies at least qualitatively
Sekanina's nucleus model of P/Tempel 2. Even the coma morphology
observed on 17/5/88 was reproduced remarkably well, although in
this case the fan axis does not coincide with the projected
rotation axis direction.
An even more realistic modelling (based on the updated nucleus
model of P/Tempel 2; Sekanina, 1991) may lead to a better
quantitative agreement (isophote pattern} of the observed and
simulated coma images. The software may also be applied to
predict interesting viewing geometries of the coma of P/Tempel 2
which can be used to check the long-term stability of Sekanina's
nucleus model during forthcoming apparitions.
4. Acknowledqement
We like to thank Dr. T. Richtler of the Astronomical Institute
of the University of Bonn, Germany, for providing us with the
CCD observation of P/Tempel 2 obtained on 7/11/88.
5. References
A'Hearn, M.F. et al.: 1986, Nature 324, 649-651
Boehnhardt, H. et al.: 1998, icarus 86, 58-68
Cochran, A.: 1991, private communication during this conference
Jewitt, D., Luu, J.: 1989, Astron.J, 97, 1766-179%
Massonne, L.: 1986, PhD thesis, Univ. of Heidelberg
Richtler, T.: 1989, private communication
Sekanina, Z.: 1979, Icarus 27, 420-442
Sekanina, Z.: 1987, ESA SP-278, 315-336
Sekanina, Z.: 1988, IAU Ci_. 4624
Sekanina, Z.: 1991, Astron,J_ 102, 350-388
Weiss, M.: 1989, Diploma thesis, Univ. of Erlangen
West, R.: 1988, ESO Messenger 54, 55-56
Wisniewski, W.: 199%, Icarus 86, 52-57


Comet P/Tempel: Some highlights and conclusions from the 1988 apparition

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