Peculiar Chemical Abundances in the Starburst Galaxy M82 and Hypernova Nucleosynthesis

Umeda, Hideyuki; Nomoto, Ken’ichi; Tsuru, Takeshi Go; Matsumoto, Hironori

doi:10.1086/342650

Cited by 33 publications

(24 citation statements)

References 31 publications

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“…The less abundant O relative to Ne might imply that the progenitor is very massive, > 20 M (Umeda et al 2002). Umeda et al (2002) also insists that fast convective mixing in the progenitor star (Spruit 1992) creates more Ne and less O. Therefore, we concluded that the progenitor of DEM L241 was a very massive star.…”

Section: Diffuse Emissionmentioning

confidence: 76%

A detailed observation of a LMC supernova remnant DEM L241 withXMM-Newton

Bamba¹,

Ueno²,

Nakajima

et al. 2006

A&A

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We report on an XMM-Newton observation of the supernova remnant (SNR) DEM L241 in the Large Magellanic Cloud. In the soft band image, the emission shows an elongated structure, like a killifish, with a central compact source. The compact source is point-like, and named XMMU J053559.3−673509. The source spectrum is reproduced well by a power-law model with a photon index of Γ = 1.57 (1.51-1.62); and the intrinsic luminosity is 2.2 × 10 35 erg s −1 in the 0.5-10.0 keV band, with an assumed distance of 50 kpc. The source has neither significant coherent pulsations in 2.0 × 10 −3 -8.0 Hz nor time variabilities. Its luminosity and spectrum suggest that the source might be a pulsar wind nebula (PWN) in DEM L241. The spectral feature classifies this source as rather bright and hard PWN, which is similar to those in Kes 75 and B0540−693. The elongated diffuse structure can be divided into a "Head" and "Tail", and both have soft and line-rich spectra. Their spectra are reproduced well by a plane-parallel shock plasma (vpshock) model with a temperature of 0.3-0.4 keV, over-abundance in O and Ne, and a relative under-abundance in Fe. Such an abundance pattern and the morphology imply both that the emission is from the ejecta of the SNR and that the progenitor of DEM L241 is a very massive star, more than 20 M . This result is also supported by the existence of the central point source and an OB star association, LH 88. The total thermal energy and plasma mass are ∼4 × 10 50 erg and ∼200 M , respectively.

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Section: Diffuse Emissionmentioning

confidence: 76%

A detailed observation of a LMC supernova remnant DEM L241 withXMM-Newton

Bamba¹,

Ueno²,

Nakajima

et al. 2006

A&A

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“…The O underabundance measured in the hot gas cannot be modeled with standard nucleosynthesis from the present generation of SNe II. Umeda et al (2002) suggested explosive nucleosynthesis in core-collapse hypernovae, but they predicted a large underabundance of Ne and Mg as well, which is not observed.…”

Section: Discussionmentioning

confidence: 95%

“…The first attempt to measure hot-gas-phase abundances in M82 has been made quite recently by Ptak et al (1997) and slightly revised by Umeda et al (2002), by analyzing ASCA X-ray (0.4-10.0 keV) spectra. Fe and O abundances as low as 1=20 solar and significantly higher (by a factor between 3 and 10) Si, S, Mg, and Ca ones have been obtained, also consistent with BeppoSAX results (Cappi et al 1999).…”

Section: Nebular Abundances Of M82 From the Literaturementioning

confidence: 99%

Stellar and Gaseous Abundances in M82

Origlia

Ranalli

Comastri

et al. 2004

ApJ

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The near-infrared (near-IR) absorption spectra of starburst galaxies show several atomic and molecular lines from red supergiants that can be used to infer reliable stellar abundances. The metals locked in stars give a picture of the galaxy metallicity prior to the last burst of star formation. The enrichment of the new generation of stars born in the last burst can be traced by measuring the hot gas in the X-rays. For the first time, detailed stellar abundances in the nuclear region of the starburst galaxy M82 have been obtained. They are compared with those of the hot gas, as derived from an accurate reanalysis of the XMM-Newton and Chandra nuclear X-ray spectra. The cool stars and the hot gas suggest Fe=H ½ ¼À0:35 AE 0:2 dex and an overall [Si / Fe] and [Mg / Fe] enhancement by $0.4 and 0.5 dex, respectively. This is consistent with a major chemical enrichment by Type II supernova explosions in recursive bursts on short timescales. Oxygen is more puzzling to interpret, since it is enhanced by $0.3 dex in stars and depleted by $0.2 dex in the hot gas. None of the standard enrichment scenarios can fully explain such a behavior compared with that of the other -elements.

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“…Then more O, C, Al are burned to produce a larger amount of burning products such as Si, S, and Ar. Therefore, hypernova nucleosynthesis is characterized by large abundance ratios of [Si,S/O], which can explain the abundance feature of M82 (110). The mixing region is enclosed with the dotted line at M mix (out).…”

Section: Energy Dependencementioning

confidence: 99%

Nucleosynthesis yields of core-collapse supernovae and hypernovae, and galactic chemical evolution

Nomoto¹,

Tominaga²,

Umeda³

et al. 2006

Nuclear Physics A

Self Cite

783

982

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We present new nucleosynthesis yields as functions of the stellar mass, metallicity, and explosion energy (corresponding to normal supernovae and Hypernovae). We apply the results to the chemical evolution of the solar neighborhood. Our new yields are based on the new developments in the observational/theoretical studies of supernovae (SNe) and extremely metal-poor (EMP) stars in the halo, which have provided excellent opportunities to test the explosion models and their nucleosynthesis. We use the light curve and spectra fitting of individual SN to estimate the mass of the progenitor, explosion energy, and produced 56 Ni mass. Comparison with the abundance patterns of EMP stars has made it possible to determine the model parameters of core-collapse SNe, such as mixing-fallback parameters.More specifically, we take into account the two distinct new classes of massive SNe: 1) very energetic Hypernovae, whose kinetic energy (KE) is more than 10 times the KE of normal core-collapse SNe, and 2) very faint and low energy SNe (Faint SNe). These two new classes of SNe are likely to be "black-hole-forming" SNe with rotating or non-rotating black holes. Nucleosynthesis in Hypernovae is characterized by larger abundance ratios (Zn,Co,V,Ti)/Fe and smaller (Mn,Cr)/Fe than normal SNe, which can explain the observed trends of these ratios in EMP stars. Nucleosynthesis in Faint SNe is characterized by a large amount of fall-back, which explains the abundance pattern of the most Fe-poor stars. These comparisons suggest that black-hole-forming SNe made important contributions to the early Galactic (and cosmic) chemical evolution.

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Peculiar Chemical Abundances in the Starburst Galaxy M82 and Hypernova Nucleosynthesis

Cited by 33 publications

References 31 publications

A detailed observation of a LMC supernova remnant DEM L241 withXMM-Newton

A detailed observation of a LMC supernova remnant DEM L241 withXMM-Newton

Stellar and Gaseous Abundances in M82

Nucleosynthesis yields of core-collapse supernovae and hypernovae, and galactic chemical evolution

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