dc.creator | Cooke, Ryan J. | |
dc.creator | Noterdaeme, Pasquier | |
dc.creator | Johnson, James W. | |
dc.creator | Pettini, Max | |
dc.creator | Welsh, Louise | |
dc.creator | Peroux, Celine | |
dc.creator | Murphy, Michael T. | |
dc.creator | Weinberg, David H. | |
dc.date.accessioned | 2022-11-16T18:32:32Z | |
dc.date.accessioned | 2023-05-18T23:24:21Z | |
dc.date.available | 2022-11-16T18:32:32Z | |
dc.date.available | 2023-05-18T23:24:21Z | |
dc.date.created | 2022-11-16T18:32:32Z | |
dc.date.issued | 2022 | |
dc.identifier | The Astrophysical Journal, 932:60 (17pp), 2022 | |
dc.identifier | 10.3847/1538-4357/ac6503 | |
dc.identifier | https://repositorio.uchile.cl/handle/2250/189231 | |
dc.identifier.uri | https://repositorioslatinoamericanos.uchile.cl/handle/2250/6296946 | |
dc.description.abstract | We report the first direct measurement of the helium isotope ratio, He-3/He-4, outside of the Local Interstellar Cloud, as part of science-verification observations with the upgraded CRyogenic InfraRed Echelle Spectrograph. Our determination of He-3/He-4 is based on metastable He I* absorption along the line of sight toward Theta(2)A Ori in the Orion Nebula. We measure a value He-3/He-4 = (1.77 +/- 0.13) x 10(-4) , which is just similar to 40% above the primordial relative abundance of these isotopes, assuming the Standard Model of particle physics and cosmology, (He-3/He-4)(p) = (1.257 +/- 0.017) x 10(-4). We calculate a suite of galactic chemical evolution simulations to study the Galactic build up of these isotopes, using the yields from Limongi & Chieffi for stars in the mass range M = 8-100 M-circle dot and Lagarde et al. for M = 0.8-8 M-circle dot. We find that these simulations simultaneously reproduce the Orion and protosolar He-3/He-4 values if the calculations are initialized with a primordial ratio (He-3/He-4)(p) = (1.043 +/- 0.089) x 10(-4). Even though the quoted error does not include the model uncertainty, this determination agrees with the Standard Model value to within similar to 2 sigma. We also use the present-day Galactic abundance of deuterium (D/H), helium (He/H), and He-3/He-4 to infer an empirical limit on the primordial He-3 abundance, (He-3/H)(p) <= (1.09 +/- 0.18) x 10(-5), which also agrees with the Standard Model value. We point out that it is becoming increasingly difficult to explain the discrepant primordial Li-7/H abundance with nonstandard physics, without breaking the remarkable simultaneous agreement of three primordial element ratios (D/H, He-4/H, and He-3/He-4) with the Standard Model values. | |
dc.language | en | |
dc.publisher | IOP | |
dc.rights | http://creativecommons.org/licenses/by-nc-nd/3.0/us/ | |
dc.rights | Attribution-NonCommercial-NoDerivs 3.0 United States | |
dc.source | The Astrophysical Journal | |
dc.subject | Bank telescope observations | |
dc.subject | Stellar evolution | |
dc.subject | Noble-gases | |
dc.subject | Deuterium abundance | |
dc.subject | Star-formation | |
dc.subject | Main-sequence | |
dc.subject | Mass | |
dc.subject | Milky | |
dc.subject | Absorption | |
dc.subject | Models | |
dc.title | Primordial helium-3 redux : the helium isotope ratio of the Orion nebula | |
dc.type | Artículo de revista | |