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IIntroductionComet 12P/Pons-Brooks is a Halley-type comet discovered in 1812. Returning every 71 years from just beyond the orbit of Neptune, outbursts were reported during each of its apparitions since. On its way to its most recent perihelion passage (21/04/2024) the comet exhibited large outbursts, such as on 20/07/2023 (magnitude 17 to12) or 14/11/2023 (magnitude 14 to9), with several smaller outbursts in between.Outbursts can be linked to mechanical processes (e.g fragmentation), external phenomena (e.g collisions) or internal physico-chemical processes (e.g. crystallisation of ice)1. Regular outbursts on 12P might indicate that its structure or make-up are to blame. The 2024 return of the comet presented a perfect opportunity to study its composition and behaviour.IIMethods Long slit spectra of 12P were acquired with the Isaac Newton Telescope(INT) IDS on 23/08/2023, 17-18/11/2023, and with the Nordic Optical telescope(NOT) ALFOSC on 17/12/2023. They cover the spectral range 304-640nm for INT-IDS and 350-535nm for NOT-ALFOSC, probing emission regions of common radicals such as CN, C2, C3, etc. We calculated molecular production rates Q and upper limits of OH, NH, CN, C2and C3 by comparing the integrated flux within a 10000km distance from the nucleus to a standard Haser model. We used a gas velocity of v=1km/s as well as commonly used scale-lengths and fluorescence factors. We also produced column density profiles of CN, C2and C3along the spectrograph slit (aligned with the parallactic angle). These can help searching for features, studying the release mechanisms of species by comparing them to models, etc.IIIResultsBased on our observations (e.g. Fig. 1), the composition of 12P (Table 1) seems typical, although slightly carbon-depleted (average Q(C2)/Q(CN)=0.9130.053) and slightly low in OH compared to other radicals. Abundance ratios do not seem to vary significantly from November to December and seem in agreement with preliminary production rates from the TRAPPIST telescopes (e.g. 2). Paired with these measurements, our observations from November show a decline of the 14/11/2023 outburst gas release within a few days. In November, we measure slightly asymmetrical profiles for C2, C3 and CN. In December, the asymmetry is even stronger (Fig. 2). This is consistent with multiple reports of a complex coma morphology (e.g 3). A faint feature is visible in the CN profile on 17/11/2023, which could be a minor outburst amidst the large 14/11/2023 outburst. While C2and C3would be expected to have similar release mechanisms, the C2profiles look particularly flat while C3and CN look more peaked, perhaps indicating a separate origin. As illustrated by Fig. 3, the expected Haser model with empirical scale-lengths fails to reproduce the observed profiles. For all profiles, adjusting the model with variable scale-lengths and Q values returns parent and daughter scale-lengths that are close to equal. These parameters translate into profile shapes in log-scale that are more angular (flat then sharply decreasing) than expected with the Haser model and usual parameters. Such shapes can also be obtained by more complex Haser models such as three-generation or grain-halo models4. This could suggest the presence of extended sources in the coma, especially for C2which seems to behave unusually. With the Q values found by adjusting the Haser model parameters to the profiles, the comet does not seem carbon-depleted anymore. While the adjusted profiles still do not exactly match the observations (especially for C2), this highlights the complexity of composition measurements and classification for unusual comets for which the standard model may not apply.Figure 1 Average INT-IDS optical spectrum of comet 12P on 17/11/2023, integrated within 10000km from the nucleus, showing detection of emission lines from several species. 23/08/2023 17/11/2023 18/11/2023 17/12/2023 QOH 1028 s-1
Ferellec et al. (Wed,) studied this question.