First Detection of 3He+ in the Planetary Nebula IC 418

Lizette Ramirez; J R Rizzo; Albert Zijlstra; C Garcia-Miro; C Morisset; Malcolm Gray

doi:10.1093/mnrasl/slw070

First Detection of 3He+ in the Planetary Nebula IC 418

Lizette Ramirez, J R Rizzo, Albert Zijlstra, C Garcia-Miro, C Morisset, Malcolm Gray

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Abstract

The ³He isotope is important to many fields of astrophysics, including stellar evolution, chemical evolution, and cosmology. The isotope is produced in low-mass stars which evolve through the planetary nebula (PN) phase. ³He abundances in PNe can help test models of the chemical evolution of the Galaxy. We present the detection of the ³He+ emission line using the single dish Deep Space Station 63, towards the PN IC 418.We derived a ³He/H abundance in the range 1.74 ± 0.8 ± 10^-3 to 5.8 ± 1.7 ± 10^-3, depending on whether part of the line arises in an outer ionized halo. The lower value for ³He/H ratio approaches values predicted by stellar models which include thermohaline mixing, but requires that large amounts of ³He are produced inside low-mass stars which enrich the interstellar medium (ISM). However, this overpredicts the ³He abundance in H II regions, the ISM, and protosolar grains, which is known to be of the order of 10^-5. This discrepancy questions our understanding of the evolution of the ³He, from circumstellar environments to the ISM.

Original language	English
Pages (from-to)	L35-L39
Number of pages	5
Journal	Monthly Notices of the Royal Astronomical Society: Letters
Volume	460
Issue number	1
Early online date	12 Apr 2016
DOIs	https://doi.org/10.1093/mnrasl/slw070
Publication status	Published - 21 Jul 2016

Keywords

abundances - circumstellar matter - planetary nebulae
IC 418 - radio lines
Individual
nuclear reactions
nucleosynthesis
stars

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10.1093/mnrasl/slw070

1604.02679v1_loggedAccepted author manuscript, 191 KB

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title = "First Detection of 3He+ in the Planetary Nebula IC 418",

abstract = "The 3He isotope is important to many fields of astrophysics, including stellar evolution, chemical evolution, and cosmology. The isotope is produced in low-mass stars which evolve through the planetary nebula (PN) phase. 3He abundances in PNe can help test models of the chemical evolution of the Galaxy. We present the detection of the 3He+ emission line using the single dish Deep Space Station 63, towards the PN IC 418.We derived a 3He/H abundance in the range 1.74 ± 0.8 ± 10-3 to 5.8 ± 1.7 ± 10-3, depending on whether part of the line arises in an outer ionized halo. The lower value for 3He/H ratio approaches values predicted by stellar models which include thermohaline mixing, but requires that large amounts of 3He are produced inside low-mass stars which enrich the interstellar medium (ISM). However, this overpredicts the 3He abundance in H II regions, the ISM, and protosolar grains, which is known to be of the order of 10-5. This discrepancy questions our understanding of the evolution of the 3He, from circumstellar environments to the ISM.",

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AU - Morisset, C

AU - Gray, Malcolm

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N2 - The 3He isotope is important to many fields of astrophysics, including stellar evolution, chemical evolution, and cosmology. The isotope is produced in low-mass stars which evolve through the planetary nebula (PN) phase. 3He abundances in PNe can help test models of the chemical evolution of the Galaxy. We present the detection of the 3He+ emission line using the single dish Deep Space Station 63, towards the PN IC 418.We derived a 3He/H abundance in the range 1.74 ± 0.8 ± 10-3 to 5.8 ± 1.7 ± 10-3, depending on whether part of the line arises in an outer ionized halo. The lower value for 3He/H ratio approaches values predicted by stellar models which include thermohaline mixing, but requires that large amounts of 3He are produced inside low-mass stars which enrich the interstellar medium (ISM). However, this overpredicts the 3He abundance in H II regions, the ISM, and protosolar grains, which is known to be of the order of 10-5. This discrepancy questions our understanding of the evolution of the 3He, from circumstellar environments to the ISM.

AB - The 3He isotope is important to many fields of astrophysics, including stellar evolution, chemical evolution, and cosmology. The isotope is produced in low-mass stars which evolve through the planetary nebula (PN) phase. 3He abundances in PNe can help test models of the chemical evolution of the Galaxy. We present the detection of the 3He+ emission line using the single dish Deep Space Station 63, towards the PN IC 418.We derived a 3He/H abundance in the range 1.74 ± 0.8 ± 10-3 to 5.8 ± 1.7 ± 10-3, depending on whether part of the line arises in an outer ionized halo. The lower value for 3He/H ratio approaches values predicted by stellar models which include thermohaline mixing, but requires that large amounts of 3He are produced inside low-mass stars which enrich the interstellar medium (ISM). However, this overpredicts the 3He abundance in H II regions, the ISM, and protosolar grains, which is known to be of the order of 10-5. This discrepancy questions our understanding of the evolution of the 3He, from circumstellar environments to the ISM.

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First Detection of 3He+ in the Planetary Nebula IC 418

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