A Spectroscopic Study of Nuclear Processing and the Production of Anomalously Strong Lines in the Crab Nebula

MacAlpine, G. M.; Ecklund, Tait; Lester, William; Strolger, L. G.

doi:10.1086/509504

Cited by 17 publications

(15 citation statements)

References 32 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…2), A as also seen in the Crab Nebula (MacAlpine et al 2007). From the spectrum synthesis ( § 3.5), we find that this feature is reproduced by [Ni ii] l7380 if the mass of Ni is ∼0.05…”

Section: Introductionsupporting

confidence: 68%

SN 2006aj Associated with XRF 060218 at Late Phases: Nucleosynthesis Signature of a Neutron Star-driven Explosion

Maeda

Kawabata

Tanaka

et al. 2007

ApJ

100

View full text Add to dashboard Cite

Optical spectroscopy and photometry of SN 2006aj have been performed with the Subaru telescope at t 1 days after GRB 060218, the X-ray flash with which it was associated. Strong nebular emission lines with 200 an expansion velocity of km s were detected. The peaked but relatively broad [O i] ll6300, 6363 Ϫ1 v ∼ 7300 suggests the existence of ∼2 of materials in which ∼1.3 is oxygen. The core might be produced by a M M , , mildly asymmetric explosion. The spectra are unique among SNe Ic in (1) the absence of [Ca ii] ll7291, 7324 emission and (2) a strong emission feature at ∼7400 , which requires ∼0.05 of newly synthesized 58 Ni. A M , Such a large amount of stable neutron-rich Ni strongly indicates the formation of a neutron star. The progenitor and the explosion energy are constrained to and ergs, respectively. 51 18 M Շ M Շ 22 M E∼ (1-3) # 10

show abstract

“…2), A as also seen in the Crab Nebula (MacAlpine et al 2007). From the spectrum synthesis ( § 3.5), we find that this feature is reproduced by [Ni ii] l7380 if the mass of Ni is ∼0.05…”

Section: Introductionsupporting

confidence: 68%

SN 2006aj Associated with XRF 060218 at Late Phases: Nucleosynthesis Signature of a Neutron Star-driven Explosion

Maeda

Kawabata

Tanaka

et al. 2007

ApJ

100

View full text Add to dashboard Cite

show abstract

“…The [Ni II] λ7378 line is one of the strongest lines emitted by the Crab nebula, with the Ni/Fe ratio estimated to be 60 − 75 times the solar value (MacAlpine et al 1989(MacAlpine et al , 2007. The variation with spatial position is relatively small, and imaging shows the nickel and iron lines to arise from the same filaments (MacAlpine et al 1989;Hester et al 1990).…”

Section: Discussion and Summarymentioning

confidence: 99%

Supersolar Ni/Fe production in the Type IIP SN 2012ec

Jerkstrand

Smartt

Sollerman

et al. 2015

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

SN 2012ec is a Type IIP supernova (SN) with a progenitor detection and comprehensive photospheric-phase observational coverage. Here, we present Very Large Telescope and PESSTO observations of this SN in the nebular phase. We model the nebular [O I] λλ6300, 6364 lines and find their strength to suggest a progenitor main-sequence mass of 13 − 15 M ⊙ . SN 2012ec is unique among hydrogen-rich SNe in showing a distinct line of stable nickel [Ni II] λ7378. This line is produced by 58 Ni, a nuclear burning ash whose abundance is a sensitive tracer of explosive burning conditions. Using spectral synthesis modelling, we use the relative strengths of [Ni II] λ7378 and [Fe II] λ7155 (the progenitor of which is 56 Ni) to derive a Ni/Fe production ratio of 0.20 ± 0.07 (by mass), which is a factor 3.4 ± 1.2 times the solar value. High production of stable nickel is confirmed by a strong [Ni II] 1.939 µm line. This is the third reported case of a core-collapse supernova producing a Ni/Fe ratio far above the solar value, which has implications for core-collapse explosion theory and galactic chemical evolution models.

show abstract

“…Thus ejection from a neutron star is unlikely. However, it has been suggested that radiation-driven winds during photospheric radius expansion may lead to ejection of a tiny fraction of the envelope (containing nuclear processed material; see Weinberg et al 2006;MacAlpine et al 2007). Indeed, XRBs have been proposed as a possible source of the light p-nuclei 92,94 Mo and 96,98 Ru (Schatz et al 1998(Schatz et al , 2001.…”

Section: Comparison With Previous Workmentioning

confidence: 99%

Hydrodynamic Models of Type I X-Ray Bursts: Metallicity Effects

José

Moreno

Parikh

et al. 2010

ApJS

112

View full text Add to dashboard Cite

Type I X-ray bursts are thermonuclear stellar explosions driven by chargedparticle reactions. In the regime for combined H/He-ignition, the main nuclear flow is dominated by the rp-process (rapid proton-captures and β + -decays), the 3α-reaction, and the αp-process (a suite of (α,p) and (p,γ) reactions). The main flow is expected to proceed away from the valley of stability, eventually reaching the proton drip-line beyond A = 38. Detailed analysis of the relevant reactions along the main path has only been scarcely addressed, mainly in the context of parameterized one-zone models. In this paper, we present a detailed study of the nucleosynthesis and nuclear processes powering type I X-ray bursts. The reported 11 bursts have been computed by means of a spherically symmetric (1D), Lagrangian, hydrodynamic code, linked to a nuclear reaction network that contains 325 isotopes (from 1 H to 107 Te), and 1392 nuclear processes. These evolutionary sequences, followed from the onset of accretion up to the explosion and expansion stages, have been performed for 2 different metallicities to explore the dependence between the extension of the main nuclear flow and the initial metal content. We carefully analyze the dominant reactions and the products of nucleosynthesis, together with the the physical parameters that determine the light curve (including recurrence times, ratios between persistent and burst luminosities, or the extent of the envelope expansion). Results are in qualitative agreement with the observed properties of some well-studied bursting sources. Leakage from the predicted SbSnTe-cycle cannot be discarded in some of our models. Production of 12 C (and implications for the mechanism that powers superbursts), light p-nuclei, and the amount of H left over after the bursting episodes will also be discussed.

show abstract

A Spectroscopic Study of Nuclear Processing and the Production of Anomalously Strong Lines in the Crab Nebula

Cited by 17 publications

References 32 publications

SN 2006aj Associated with XRF 060218 at Late Phases: Nucleosynthesis Signature of a Neutron Star-driven Explosion

SN 2006aj Associated with XRF 060218 at Late Phases: Nucleosynthesis Signature of a Neutron Star-driven Explosion

Supersolar Ni/Fe production in the Type IIP SN 2012ec

Hydrodynamic Models of Type I X-Ray Bursts: Metallicity Effects

Contact Info

Product

Resources

About