A Remarkable 3 Hour Thermonuclear Burst from 4U 1820–30

By T. Strohmayer, E. Brown. 2001

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We present a detailed observational and theoretical study of a ~3 hr long X-ray burst (the "superburst") observed by the Rossi X-Ray Timing Explorer (RXTE) from the low-mass X-ray binary 4U 1820-30. This is the longest X-ray burst ever observed from this source and perhaps one of the longest ever observed in great detail from any source. We show that the superburst is thermonuclear in origin. Its peak luminosity of ~3.4 × 1038 ergs s-1 is consistent with the helium Eddington limit for a neutron star at ~7 kpc as well as the peak luminosity of other, shorter, thermonuclear bursts from the same source. The superburst begins in the decaying tail of a more typical (≈20 s duration) thermonuclear burst. These shorter, more frequent bursts are well-known helium flashes from this source. The level of the accretion-driven flux as well as the observed energy release of upward of 1.5 × 1042 ergs indicate that helium could not be the energy source for the superburst. We outline the physics relevant to carbon production and burning on helium-accreting neutron stars and present calculations of the thermal evolution and stability of a carbon layer and show that this process is the most likely explanation for the superburst. Ignition at the temperatures in the deep carbon "ocean" requires more than 30 times the mass of carbon inferred from the observed burst energetics unless the He flash is able to trigger a deflagration from a much smaller mass of carbon. We show, however, that for large columns of accreted carbon fuel, a substantial fraction of the energy released in the carbon-burning layer is radiated away as neutrinos, and the heat that is conducted from the burning layer in large part flows inward, only to be released on timescales longer than the observed burst. Thus, the energy released during the event possibly exceeds that observed in X-rays by more than a factor of 10, making the scenario of burning a large mass of carbon at great depths consistent with the observed fluence without invoking any additional trigger. A strong constraint on this scenario is the recurrence time: to accrete an ignition column of 1013 g cm-2 takes ~13/(/3 × 1017 g s-1) yr. Spectral analysis during the superburst reveals the presence of a broad emission line between 5.8 and 6.4 keV and an edge at 8-9 keV, likely due to reflection of the burst flux from the inner accretion disk in 4U 1820-30. We believe that this is the first time such a signature has been unambiguously detected in the spectrum of an X-ray burst.

Subfields: Astronomy and Astrophysics, Biomedical Engineering, Geophysics

View Paper: https://www.semanticscholar.org/paper/01ed523d3866908d9d6aba0d5661fb5992482a1f

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Citations in the corpus

Thermonuclear Burst Oscillations (2012, background): “Superbursts are thought to be caused by unstable burning of carbon (Woosley & Taam 1976, Taam & Picklum 1978, Brown & Bildsten 1998, Cumming & Bildsten 2001, Strohmayer & Brown 2002).”
Long Type I X-Ray Bursts and Neutron Star Interior Physics (2005, methodology): “The time between the previous superburst and the superburst observed by RXTE PCA was 1.75 yr (Kuulkers et al. 2004).”
INTEGRAL observations of recurrent fast X-ray transient sources (2005, background): “It is worth noting that even longer type I X-ray bursts exist, the so-called superbursts, lasting for several hours (Cornelisse et al. 2000, 2002; Wijnands 2001; Strohmayer & Brown 2002; Kuulkers 2001; Kuulkers et al. 2002).”
Photospheric radius expansion X-ray bursts as standard candles (2002, methodology): “…which were similar to that reported during the photospheric radius expansion phases of the strong X-ray burst from 4U2129+12 seen by the Ginga/LAC (van Paradijs et al. 1990), the long X-ray bursts seen from GX17+2 (Kuulkers et al. 2002), and the superburst from 4U1820−30 (Strohmayer & Brown 2002).”
THE MASS AND RADIUS OF THE NEUTRON STAR IN 4U 1820−30 (2010, background): “4U1820−30 also exhibited a super-burst during RXTE observations (Strohmayer & Brown 2002), most probably resulting from a burning of a large mass of carbon.”
THE JINA REACLIB DATABASE: ITS RECENT UPDATES AND IMPACT ON TYPE-I X-RAY BURSTS (2010, background): “…et al. 1986; Watts & Maurer 2007), the unexplained burst behavior at high accretion rates (Kuulkers et al. 2002; Cornelisse et al. 2003), or the origin of 12C in the burst ashes thought to be required to power the rarely observed superbursts (Cumming & Bildsten 2001; Strohmayer & Brown 2002).”
Models for Type I X-Ray Bursts with Improved Nuclear Physics (2003, background): “These flashes have 1000 times the energy and duration of normal Type I bursts, and have been interpreted as unstable ignition of a thick carbon layer (Cumming & Bildsten 2001; Strohmayer & Brown 2002), originally proposed by Woosley & Taam (1976) as a gamma-ray burst model.”