Issue |
A&A
Volume 495, Number 3, March I 2009
|
|
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Page(s) | 975 - 978 | |
Section | Planets and planetary systems | |
DOI | https://doi.org/10.1051/0004-6361:200810458 | |
Published online | 20 January 2009 |
Why did Comet 17P/Holmes burst out?
Nucleus splitting or delayed sublimation?
W. J. Altenhoff1 - E. Kreysa1 - K. M. Menten1 - A. Sievers3 - C. Thum2 - A. Weiss1
1 - Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69,
53121 Bonn, Germany
2 -
IRAM, University campus, 38406 St. Martin d'Herès, France
3 -
IRAM, Pico Veleta, Granada, Spain
Received 25 June 2008 / Accepted 15 December 2008
Abstract
Based on millimeter-wavelength
continuum observations we suggest
that the recent ``spectacle'' of comet 17P/Holmes
can be explained by a thick, air-tight
dust cover and the effects of H2O sublimation, which started when the comet
arrived at the heliocentric distance
2.5 AU. The porous
structure inside the nucleus provided enough surface for additional
sublimation, which eventually led to the break up of the dust cover and
to the observed outburst. The magnitude of the particle burst can be explained
by the energy provided by insolation, stored in the dust cover and the nucleus
within the months before the outburst: the subliming surface
within the nucleus is more than one order of magnitude larger
than the geometric surface of the nucleus -
possibly an indication of the latter's porous structure.
Another surprise is that the abundance ratios of
several molecular species with respect to
H2O are variable.
During this apparition, comet Holmes lost about 3
of its mass,
corresponding to a ``dirty ice'' layer of 20 m.
Key words: comets: general - comets: individual: 17P/Holmes
1 Introduction
Comet 17P/Holmes was serendipitously discovered during an outbreak on 1892 November 6 by Holmes (reported by Plummer 1893) while he was observing the nearby Andromeda galaxy (M 31). Until early 1893 January, the comet faded from magnitude 4 to 9-10, after which a second eruption to

Montalto et al. (2008) report a significant disassembly of the nucleus, not even excluding a complete disintegration. Earlier, Sekanina (1982) had classified types of splitting comets: (a) single comets that break up into two or more; (b) comets that disintegrate or suddenly disappear; (c) and those with a pancake-shaped companion nucleus that disintegrates into microscopic dust grains. Recently, Sekanina (2008) summarized the optical observations of 17P/Holmes and some other comets for comparison. All types of splitting comets start in his hypothesis with a major outburst. The ``megaburst'' of 17P/Holmes is of type (c), starting with an exothermic reaction, resulting in a rapidly expanding cloud of microscopic dust particles. But not all major outbursts end in splitting: e.g., the one of comet Halley on 1991 February 12 at a heliocentric distance, r, of 14 AU (Sekanina et al. 1992).
2 The nucleus
2.1 Time line
The ``engine'' behind the cometary activity of Comet Holmes is the
production of gaseous water
as described by Delsemme (1982). Its
production rate, Q(H2O), is a function
of heliocentric distance. It is
1/r2for low values of r,
while for r
AU the dependence becomes
highly nonlinear. Delsemme defines the limit of sublimation r0,
the heliocentric distance beyond which
97.5% of the energy received by insolation is re-radiated,
and only
2.5% are used for vaporization. For water ice,
r0 is about 2.5 AU.
Comet Holmes is a short-period comet in the Jupiter family (a JFC).
Its average perihelion distance, q, over the last
6 apparitions was 2.2 AU (Marsden & Williams 1999),
close to the limit of H2O sublimation. But the perihelion
distance of the most recent apparition was at a q of 2.05 AU.
With the steepened production rate, mentioned
above, the H2O production is increased by a factor of 2.
This is possibly responsible for the outburst.
The outburst happened according to Hsieh et al. (2007) on 2007 October 23.8, 173 days after perihelion passage, or 361 days after crossing r = 2.5 AU. Probably - because of the low-level cometary activity - the nuclear surface was free of ice and the icy nucleus was covered by some sort of a rubble pile (Jewitt 1992) or dust-particle mantle, causing the delay of visible cometary sublimation by months. During this period, the dust cover was ``air tight'', preventing the sublimated gas to escape. Sublimation inside the nucleus continued until the gas set free by this process broke up the dust mantle - the ``outburst''.
2.2 Model parameter
Dust cover. All accurately measured cometary nuclei show a geometric albedo, pbetween 0.02
and 0.05 (see e.g. Jewitt 2005), which is indicative of a dust cover.
If closely packed, this material is thought to have
a density,
1 g cm-3, as inferred from numerous
radar observations (Harmon 1999; Harmon et al. 2005).
Information from the collision caused by the Deep Impact mission revealed that
the nucleus of comet Tempel 1
had a devolatilized dust cover of about 1 m, with very little H2O
inside and none on the outside (Sunshine et al. 2007) -
identical to what we assume for 17P/Holmes.
Below the dust cover of comet Tempel 1,
an at least 10 m thick layer of fine grained water ice particles was found,
which appeared to be free of
refractory impurities! This ``clean''
ice may originate from repeated sublimation and deposition
inside the enclosed nucleus approaching and leaving the solar neighborhood.
It is likely that comet Holmes has a similar layer.
But for our model we neglect this detail and assume for the mass estimates
``dirty'' amorphous H2O ice throughout the nucleus.
Diameter. Until recently, the resolution of optical
telescopes was not high enough to directly measure the nuclear diameters
of JFCs. Instead, absolute magnitudes of the nuclei were
determined and nuclear diameters were calculated, assuming a geometric
albedo p = 0.04, because observations constrain the albedo to
(see e.g. Jewitt 2005).
For 17P/Holmes an absolute magnitude, H
,
of 16.6 (Tankredi 2006)
was found and a median nuclear diameter,
,
of 3.2 km derived within the
limits of 4.6 and 2.9 km, corresponding to the albedo range.
Meanwhile, Lamy et al. (2005)
report a diameter
km, obtained by a single
snapshot by the Hubble space telescope (HST). We prefer this direct measurement,
even though it might need a correction, if the nucleus is not spherical.
Bulk density, porosity. The bulk density may change from
comet to comet, depending, e.g., on the outgassing history. For our model
the value
= 0.5 g cm-3 was selected, derived by
Rickman (1989) for the comet Halley data and
from observations of 29 short period comets by Rickman et al. (1987).
For the porosity (fraction of void volume/bulk volume)
we assume a value 0.60. This provides ample storage for sublimated molecular
gas inside the nucleus.
Equilibrium temperature.
One needs to know the brightness temperature, ,
of the nucleus and
the dust grains to calculate their emission. In the absence of new data, we assume
that they both will be close to the equilibrium temperature,
.
For a heliocentric distance of r
2.45 AU and an albedo p
of 0.04, we assume
175 K, i.e., identical to
.
3 Observations
Table 1:
Flux densities
at 250 GHz in a 11'' beam of 17P/Holmes.
and r are the comet's distance from Earth and Sun
at time T after the outbreak.
The outburst of comet 17P/Holmes came at an unfavorable moment, when on Pico Veleta the MAx-Planck Millimeter BOlometer array (MAMBO) had not been installed on the 30 m telescope; in Effelsberg the 9 mm wavelength receiver was not operational at the 100 m telescope; and for the Atacama Pathfinder EXperiment (APEX) 12 m telescope, the comet was below the declination limit. About 25 days later, when MAMBO went back into operation, we started a series of maps and ON/OFF observations at its effective frequency of 250 GHz, trying to see the aftermath of the outburst. The observing and evaluation procedures of MAMBO observations are standard routines and have been frequently reported; see e.g. Altenhoff et al. (2000).
The results are collected in Table 1.
Prior to our measurements, the comet had already been detected
with the Plateau de Bure
Interferometer (PdBI) near 90 GHz by Boissier et al. (2008, 2009).
Their results, generously made available to us
prior to publication, are included in our analysis. We have scaled
the 90 GHz flux densities, obtained with a synthesized beam of
5.7 7.3 arcsec, to the angular resolution of our MAMBO data
(11 arcsec), and we extrapolated the signal to 250 GHz with the
canonical spectral index of comets SI = 2.7, reversing
the procedure of Jewitt & Matthews (1999) to derive the spectral index
of comet Hale-Bopp. This method was intensively tested by
Altenhoff et al. (2008).
Each stage of the optical development has an equivalent one at millimeter (mm) wavelengths. The optical observations are summarized in Sekanina (2008), e.g. with the total magnitude m1 as a function of time, ``the light curve''.
The mm data are compiled in Table 1 and Fig. 1. The extrapolation of the PdBI observations to 250 GHz is fairly accurate, and the combined errors of extrapolation and observation are indicated by the size of the symbols. The small beam broadening by the comet, reported by Boissier et al. (2008) shows that the source is optically thin. The two data sets are interpolated, suggesting a signal loss of 7% per day. The series of nuclear magnitudes m2 shows a similar slope.
In a separate paper, Altenhoff et al. (2008)
show that most cometary
mm/radio light curves can be represented by the following equation:

with


Thus the light curve is calculated and plotted in Fig. 1. It is obviously a reasonable fit for the time after day 33, when insolation and dust production (determining the intensity of the mm radiation) are apparently coming to equilibrium. For the first 30 days, this radio light curve is the baseline for the burst. As a further indicator of cometary activity, we use the nuclear magnitude, m2, reported with the astrometric positions (Marsden 2007). These values with limited accuracy are averaged over three days (typically over 100 observations) to reduce the noise. These data also confirm increased nuclear activity in the first 30 days. Red circles show the H2O production rates measured with the Solar Wind ANisotropy (SWAN) experiment on the SOlar Heliospheric Observatory (SOHO) reported by Combi (2007). This system has a beam of about one degree, probing the water production of about 4 days. This may be a crude guess, considering that we are using observing results obtained with very different resolutions. Even though we guess that, with the resulting smearing, the production rate might fit even better to our observed extended cometary activity.
Spectroscopic observations of HCN by Biver et al. (2008) at Pico Veleta and at the Caltech submillimeter observatory (CSO), and by Drahus et al. (2007, 2008) with the Arizona radio observatory (ARO), are shown for comparison. The data sets are consistent which each other and show a steeper decay than the cometary activity described before.
![]() |
Figure 1: Comet 17P/Holmes: compilation of spectroscopic and continuum observations. The black dots and the black diamonds represent the mm continuum data at 250 GHz, taken with the 30 m and the PdBI, respectively. Dashed line: model of mm halo (see text). Red open circles: H2O emission, observed with SWAN, light blue dots: HCN emission, blue squares: HCN emission. See text for references. The dotted magenta curve shows the optical nuclear magnitudes m2, as an indicator of the nuclear activity. The spectroscopic data sets are normalized to their respective maximum. |
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4 Mass determination
Fine dust.
Optically, the scattered light by small dust particles is dominating
the appearance of comets, even though the mass of these particles
is low. Sekanina (1982) has estimated the mass of m sized
fine dust in comet 17P/Holmes (see Table 2) near its outbreak.
The size of the scattering particles
is too small to detect with radio or mm telescopes. This dust is
responsible for the optical appearance seen at magnitude m1.
The particulate dust and the bulk of the molecular gas are almost
invisible optically.
Particulate dust.
Radio and mm continuum observations measure the thermal emission
of dust particles of size 10% of the observing wavelength, here
0.2 mm. Since the observed signal is proportional to the
integrated particle cross sections, but the particle mass is
proportional to its volume, the mass of big particles
is underestimated, so
observations at different wavelengths are needed for a more precise
mass estimate.
We estimate the dust mass with the photometric diameter to be the
size of a disk at the distance of the comet with its equilibrium
temperature, radiating as black body,
yielding the same flux density as the radio/mm halo.
For cometary dust, we find that the black body condition
(emissivity
1) is fulfilled
with a density of 1 g cm-3 and a layer depth of 3 wavelengths
(as confirmed by the rigorous halo
evaluation for comets Hyakutake and Hale-Bopp (Altenhoff et al. 2000).
This allows calculation of the dust mass in the halo for any observed signal.
Dust production rate. The average particle moves through the telescope's diffraction beam in about 60 h, and the resulting dust production rate and the dust mass in the beam are listed in Table 2.
Table 2: Mass budget.
Hypothetical pre-burst dust. The radio light curve, as defined above, can be extrapolated backwards over the whole apparition to calculate ``hypothetical'' signals and masses that would have been emitted in the absence of the dust cover. This total hypothetical mass is a factor 3-4 higher than the total mass released within 33 days after the outburst, i.e. the burst dust mass. Thus, we can safely assume that the insolation provided enough energy to start sublimation within the nucleus.
Accuracy estimate.
Within our observing interval, the mass in the halo is approximately
proportional to the observed flux density in the beam, thus to the
observing accuracy. Therefore
the relative accuracy from day to day and of the dust production rate is
quite good.
The absolute accuracy depends on our knowledge of the
absorption coefficient
of cometary dust, whose uncertainty
was estimated by Altenhoff et al. (2000) to be about a factor 2.
The accuracies of the mass determinations of the small-grained dust
(Sekanina 2007) and of water (Combi 2007) have unfortunately not
been reported.
5 Interpretation
Start of the outburst. The nuclear structure of comets 9P/Tempel 1 and 17P/Holmes before the outbursts are probably alike, a densely packed dust cover (

Time scale of the outburst. Different versions exist of the development of the outburst. Sekanina (2008, 2007) refers to an explosion and a single exothermic event, and Biver et al. (2008) and others report a water production rate, which almost ends after 3 days. In Fig. 1 the continuum observations are plotted, showing that the outburst-related increased continuum emission lasted for about 30 days, as did the increased nuclear magnitude m2. Additional proof are the numerous photographs taken within the first month of the outburst; see e.g. Sekanina (2008), in which the comet appears as a filled Plerion rather than a shell, implying that the dust injection into the coma continued after the ``explosion'' for quite some time.
Molecular production rates. Production of gas-phase molecules is responsible for all the cometary activity. It is predominantly the cometary wind of the H2O molecules, which lifts the dust particles from the nucleus, so a correlation between H2O and dust production is expected. Usually the production of different molecules shows a fixed ratio, so that one can, e.g., predict the H2O production rate from HCN observations. Not so for comet Holmes! Figure 1 shows that H2O production, observed with the SWAN satellite, lasts at least for a month as does the enhanced mm continuum emission, while e.g. the spectral lines of HCN, CO, NH3(Drahus et al. 2007; Biver et al. 2008; Menten 2007) had a big signal at the start, which apparently petered out dramatically after 3 days, as shown in Fig. 1. The reason may be the temperature/depth structure of the nucleus, because the near surface ice might be free of higher volatile molecules.
Mass comparison.
All derived masses are collected in Table 2, where the total mass and
the mass of the dust cover have been calculated with the model values.
The mass of the 2 m sized
dust, determined immediately after the outburst by Sekanina (2008),
is surprisingly high, compared to the total mass of the dust layer! Even
the total particulate dust mass (grains of size 0.2 to 7 mm) is smaller.
Integrated over the
33 days of increased cometary activity, the dust mass produced by the
outburst is
2% of the comet's total mass. Surprisingly low is also
the H2O mass released in the
first part of the outburst, when we would have expected a mass
comparable to the particulate dust
mass. The hypothetical dust mass, calculated from the radio light
curve backwards,
is about a factor of 3-4 higher than the total mass in the burst. The energy
released in the burst can be provided by the insolation before the burst,
even allowing energy losses through re-radiation by the dust cover.
The total accounted mass loss during this apparition (mass of m sized
dust, burst dust mass, burst H2O mass) is in total
3.5% of the
total nuclear mass.
If a bulk density of
= 0.5 is assumed for the outer nucleus, this
loss corresponds to a layer of 20 m thickness which is the same order
of magnitude as found from observations of other comets.
5.1 Alternative models
Sekanina (2007, 1982) explained the outburst of comet 17P/Holmes as a splitting nucleus, whereby the secondary nucleus is a fragment of a jettisoned insulation mantle of debris. The splitting starts with an exothermic event. His model considers neither particulate dust with particles
6 Conclusion
The historic outbursts, as discussed by Whipple (1986), show several similarities to the present one, suggesting that they happened the same way, but in 2 steps. After all, comet 17 P/Holmes is a comet like many others whose appearance is determined by sublimation of cometary ices. What makes it peculiar is that it had a big dust cover and that it seldom comes close enough to the Sun to afford a great display of activity. Dust covers of cometary nuclei are standard (see model of Horanyi et al. 1984) and do not indicate a splitting comet. We think that the delayed sublimation, as explained above, is a viable alternative to the theory of splitting or sudden fragmentation of the cometary nucleus.
Acknowledgements
We are grateful to Dr. J. Boissier (IRAM) for communicating the 90 GHz results to us prior to publication. We thank the director of IRAM, Dr. P. Cox, for granting special observing time and the staff on Pico Veleta, Spain, for their support of the observing program.
References
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All Tables
Table 1:
Flux densities
at 250 GHz in a 11'' beam of 17P/Holmes.
and r are the comet's distance from Earth and Sun
at time T after the outbreak.
Table 2: Mass budget.
All Figures
![]() |
Figure 1: Comet 17P/Holmes: compilation of spectroscopic and continuum observations. The black dots and the black diamonds represent the mm continuum data at 250 GHz, taken with the 30 m and the PdBI, respectively. Dashed line: model of mm halo (see text). Red open circles: H2O emission, observed with SWAN, light blue dots: HCN emission, blue squares: HCN emission. See text for references. The dotted magenta curve shows the optical nuclear magnitudes m2, as an indicator of the nuclear activity. The spectroscopic data sets are normalized to their respective maximum. |
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In the text |
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