A Rare Form of Nitrogen on Comet ISON

Subaru Telescope Detects Rare Form of Nitrogen in Comet ISON

NASA’s Hubble Space Telescope provides a close-up look of Comet ISON (C/2012 S1), as photographed on April 10, when the comet was slightly closer than Jupiter’s orbit at a distance of 386 million miles from the sun. Credit: NASA, ESA, J.-Y. Li (Planetary Science Institute), and the Hubble Comet ISON Imaging Science Team

A team of astronomers, led by Ph.D. candidate Yoshiharu Shinnaka and Professor Hideyo Kawakita, both from Kyoto Sangyo University, successfully observed the Comet ISON during its bright outburst in the middle of November 2013. Subaru Telescope’s High Dispersion Spectrograph (HDS) detected two forms of nitrogen14NH2 and 15NH2–in the comet. This is the first time that astronomers have reported a clear detection of the relatively rare isotope 15NH2 in a single comet and also measured the relative abundance of two different forms of nitrogen ("nitrogen isotopic ratio") of cometary ammonia (NH3) (Figure 1). Their results support the hypothesis that there were two distinct reservoirs of nitrogen the massive, dense cloud ("solar nebula") from which our Solar System may have formed and evolved.

Why did the team focus on studying these different forms of nitrogen in the comet? Comets are relatively small Solar System objects composed of ice and dust, which formed 4.6 billion years ago in the solar nebula when our Solar System was in its infancy. Because they usually reside in cold regions far from the Sun, e.g., the Kuiper belt and Oort cloud, they probably preserve information about the physical and chemical conditions in the early Solar System. Different forms and abundances of the same molecule provide information about their source and evolution. Were they from a stellar nursery (a primordial interstellar cloud) or from a distinctive cloud (solar nebula) that may have formed our Solar System’s star, the Sun? Scientists do not yet understand very well how cometary molecules separate into isotopes with different abundances. Isotopes of nitrogen from ammonia (NH3) may hold the key.

Figure 1: Close-up of spectra of NH2 emission lines (of the same transitions for both 14NH2 and 15NH2) in Comet ISON, showing the difference in wavelengths and relative intensity between the isotopes. The red and green-dashed lines indicate the observed spectrum. The blue line indicates 15NH2, clearly detected for the first time. Credit: NAOJ

Ammonia (NH3) is a particularly important molecule, because it is the most abundant nitrogen-bearing volatile (a substance that vaporizes) in cometary ice and one of the simplest molecules in an amino group (–NH2) closely related to life. This means that these different forms of nitrogen could link the components of interstellar space to life on Earth as we know it.

Since ammonia is the major carrier of nitrogen in a comet, it is necessary to clear it from the relative abundance of its isotopes to understand how 15NH2 separates in cometary molecules. However, the direct detection of cometary ammonia is difficult, and there are only a few reports of its clear detection. Therefore, the team concentrated on studying the form of NH2 developed after the ammonia was broken down by the light ("photodissociation") in the cometary coma. The team was fortunate to observe the comet as it neared the Sun, when its icy composition was evaporating. They were also fortunate that NH2, a derivative of ammonia (NH3), is easy to observe in the optical wavelength, and the relative abundance of nitrogen isotopes of cometary ammonia is probably close to that of NH2.

The team used Subaru Telescope’s HDS to successfully observe Comet ISON on November 15th and 16th (UT) ("Spectrum of Outburst from Comet ISON Obtained by Subaru Telescope’s High-Dispersion Spectrograph", December 2, 2013 Subaru Telescope press release), when the comet had its bright outburst that began on November 14th. The observation clearly detected 15NH2 from Comet ISON, and the team inferred that the ratio of cometary ammonia of 14N/15N (139±38) is consistent with the average (14N/15N~130) of that from the spectra of 12 other comets. In other words, Comet ISON is typical in its relative abundance of 14N/15N in cometary ammonia.

Figure 2: Comparison of nitrogen isotopic ratios obtained from comets (left) and molecular cloud core (right). The blue line indicates the ratio of nitrogen isotopes in the Earth’s atmosphere while the wider, yellow line indicates that of the protosolar nebula. The figure shows that the nitrogen isotopic ratios obtained from cometary molecules are similar to each other while those of HCN (hydrogen cyanide) and HN3 (ammonia) in the molecular cloud core are different. Credit: NAOJ

These findings support the hypothesis that there were two distinct reservoirs of nitrogen in the solar nebula: 1) primordial N2 gas having a protosolar value of 14N/15N, and 2) less volatile and probably solid molecules having a ratio of about 14N/15N~150 in the solar nebula. In the case of a dense molecular cloud core, the isotopic ratio of hydrogen cyanide (HCN) is similar to that of comets while its ratio in ammonia is different from its cometary value (Figure 2).

This may mean that the ammonia formed in an environment of a low temperature dust surface, not in the gas of the molecular cloud. Laboratory experiments show that various complex molecules can form on the surface of low temperature dust. If the ammonia molecule formed on the low temperature dust surface, the cometary nucleus could contain a complex molecule that relates to the origin of life, in addition to the ammonia. If this is so, it raises the possibility that the comet brought these materials to Earth.

In the future, the team would like to increase the sample of comets for which nitrogen isotopic ratios of cometary ammonia have been determined. They would also like to carry out laboratory measurements of 15NH2 to obtain more precise isotopic ratios. On a larger scale, the team hopes to investigate the origin of Comet ISON and the mechanisms that triggered its outburst so that we can better understand the evolution of the Solar System.


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