Evolutionary Tracks for Betelgeuse

Dolan, Michelle; Mathews, Grant J.; Lam, Doan Duc; Lan, N. Q.; Herczeg, Gregory J.; Dearborn, David S. P.

doi:10.3847/0004-637x/819/1/7

Cited by 66 publications

(72 citation statements)

References 109 publications

(188 reference statements)

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“…The mass of Betelgeuse is poorly known, and significantly different estimates can be found in the literature (see, e.g., Meynet et al 2013;Neilson et al 2011Neilson et al , 2016and Dolan et al 2016) from approximately 10 to 20 M . Assuming a mass of m Bet = 15 ± 5 M and a radius of R star = 1400 ± 250 R (from our equivalent ALMA continuum angular radius and the parallax π = 4.51 ± 0.80 mas by Harper et al 2017a), the Keplerian rotation velocity at the surface of Betelgeuse is K = 45 ± 28 km s −1 .…”

Section: Radial Rotation Velocity Profilementioning

confidence: 99%

“…The modeling efforts reported by Meynet et al (2013), Dolan et al (2016), and Wheeler et al (2017) conclude that the nearby red supergiant Betelgeuse will explode as a Type II-P or II-L supernova, but diverge significantly on its mass and evolutionary state. A major source of uncertainty of the evolutionary modeling of Betelgeuse is its rotation velocity.…”

Section: Introductionmentioning

confidence: 99%

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The close circumstellar environment of Betelgeuse

Kervella

Decin

Richards

et al. 2018

A&A

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We observed Betelgeuse using ALMA's extended configuration in band 7 ( f ≈ 340 GHz, λ ≈ 0.88 mm), resulting in a very high angular resolution of 18 mas. Using a solid body rotation model of the 28 SiO( = 2, J = 8−7) line emission, we show that the supergiant is rotating with a projected equatorial velocity of eq sin i = 5.47 ± 0.25 km s −1 at the equivalent continuum angular radius R star = 29.50 ± 0.14 mas. This corresponds to an angular rotation velocity of ω sin i = (5.6 ± 1.3) × 10 −9 rad s −1 . The position angle of its north pole is PA = 48.0 ± 3.5• . The rotation period of Betelgeuse is estimated to P/sin i = 36 ± 8 years. The combination of our velocity measurement with previous observations in the ultraviolet shows that the chromosphere is co-rotating with the star up to a radius of ≈10 au (45 mas or 1.5× the ALMA continuum radius). The coincidence of the position angle of the polar axis of Betelgeuse with that of the major ALMA continuum hot spot, a molecular plume, and a partial dust shell (from previous observations) suggests that focused mass loss is currently taking place in the polar region of the star. We propose that this hot spot corresponds to the location of a particularly strong "rogue" convection cell, which emits a focused molecular plume that subsequently condenses into dust at a few stellar radii. Rogue convection cells therefore appear to be an important factor shaping the anisotropic mass loss of red supergiants.

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Section: Radial Rotation Velocity Profilementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The close circumstellar environment of Betelgeuse

Kervella

Decin

Richards

et al. 2018

A&A

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“…As is well known, the red supergiant, Betelgeuse is one of the possible nearby galactic SN candidates with the uncertain mass and distance [46][47][48][49], e.g its distance is determined as D = 197 ± 45 pc and its mass is within M = (17 · · · 25) M in Ref. [46].…”

Section: B Sensitivitymentioning

confidence: 99%

Towards a complete reconstruction of supernova neutrino spectra in future large liquid-scintillator detectors

Li¹,

Li²,

Wang³

et al. 2018

Phys. Rev. D

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In this paper, we show how to carry out a relatively more realistic and complete reconstruction of supernova neutrino spectra in the future large liquid-scintillator detectors, by implementing the method of singular value decomposition with a proper regularization. For a core-collapse supernova at a distance of 10 kpc in the Milky Way, itsν e spectrum can be precisely determined from the inverse beta-decay processν e þ p → e þ þ n, for which a 20 kiloton liquid-scintillator detector with the resolution similar to the Jiangmen Underground Neutrino Observatory may register more than 5000 events. We have to rely predominantly on the elastic neutrino-electron scattering ν þ e − → ν þ e − and the elastic neutrino-proton scattering ν þ p → ν þ p for the spectra of ν e and ν x , where ν denotes collectively neutrinos and antineutrinos of all three flavors and ν x for ν μ and ν τ as well as their antiparticles. To demonstrate the validity of our approach, we also attempt to reconstruct the neutrino spectra by using the time-integrated neutrino data from the latest numerical simulations of delayed neutrino-driven supernova explosions.

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“…As such, it has been well studied. Betelgeuse is estimated to have a mass of 11 -20 M ⊙ (Lobel & Dupree 2001;Neilson et al 2011;Dolan et al 2016;Neilson et al 2016) ; it lies at a distance of 222 +48 −34 pc (Harper et al 2008(Harper et al , 2017, and has an age of 8 -10 Myr, with < 1 Myr of life left until core collapse (Dolan et al 2016;Harper et al 2017). We find that for D = 200 pc a presupernova neutrino signal would be practically background-free -in energy windows that are realistic for detection -for several hours, and the WO can extend up to ∼ 10 hours.…”

Section: Window Of Observabilitymentioning

confidence: 99%

Neutrinos from Beta Processes in a Presupernova: Probing the Isotopic Evolution of a Massive Star

Patton

Lunardini

Farmer

et al. 2017

ApJ

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We present a new calculation of the neutrino flux received at Earth from a massive star in the ∼ 24 hours of evolution prior to its explosion as a supernova (presupernova). Using the stellar evolution code MESA, the neutrino emissivity in each flavor is calculated at many radial zones and time steps. In addition to thermal processes, neutrino production via beta processes is modeled in detail, using a network of 204 isotopes. We find that the total produced ν e flux has a high energy spectrum tail, at E > ∼ 3 − 4 MeV, which is mostly due to decay and electron capture on isotopes with A = 50 − 60. In a tentative window of observability of E > ∼ 0.5 MeV and t < 2 hours pre-collapse, the contribution of beta processes to the ν e flux is at the level of ∼ 90% . For a star at D = 1 kpc distance, a 17 kt liquid scintillator detector would typically observe several tens of events from a presupernova, of which up to ∼ 30% due to beta processes. These processes dominate the signal at a liquid argon detector, thus greatly enhancing its sensitivity to a presupernova.

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Evolutionary Tracks for Betelgeuse

Cited by 66 publications

References 109 publications

The close circumstellar environment of Betelgeuse

The close circumstellar environment of Betelgeuse

Towards a complete reconstruction of supernova neutrino spectra in future large liquid-scintillator detectors

Neutrinos from Beta Processes in a Presupernova: Probing the Isotopic Evolution of a Massive Star

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