X-ray spectral analysis of the neutron star in SNR 1E 0102.2−7219

Hebbar, Pavan R.; Heinke, C. O.; Ho, Wynn C. G.

doi:10.1093/mnras/stz2570

Cited by 17 publications

(17 citation statements)

References 92 publications

(135 reference statements)

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“…Janka (2017) found that, for 2D and 3D simulations, a high level of explosion asymmetry (common in high mass progenitor systems) can cause higher kick velocities. Hebbar et al (2020) and Xi et al (2020) each conducted a careful analysis of Chandra observations of the candidate CCO that included time-dependent responses for each of the archival observations, modeling of the background instead of subtracting it, and fitting the unbinned spectra to preserve the maximal spectral information. Hebbar et al (2020) found that a single blackbody model does not provide an acceptable fit to the data, but a blackbody+power-law or a neutron star carbon atmosphere model do provide acceptable fits.…”

Section: Proposed Cco Resultsmentioning

confidence: 99%

“…Hebbar et al (2020) and Xi et al (2020) each conducted a careful analysis of Chandra observations of the candidate CCO that included time-dependent responses for each of the archival observations, modeling of the background instead of subtracting it, and fitting the unbinned spectra to preserve the maximal spectral information. Hebbar et al (2020) found that a single blackbody model does not provide an acceptable fit to the data, but a blackbody+power-law or a neutron star carbon atmosphere model do provide acceptable fits. However, the blackbody+power-law model fit has a neutral hydrogen column density that is ∼ 10× higher than the accepted value to E0102 and the neutron star carbon atmosphere model has a value that is ∼ 18× higher.…”

Section: Proposed Cco Resultsmentioning

confidence: 99%

“…Rutkowski et al (2010) had inspected this X-ray source using archival Chandra X-ray images to search for candidate CCOs, but did not find it to be credible. On the other hand, Hebbar et al (2020) performed X-ray spectral analysis on the source and found that it could be a neutron star powered by strong magnetic fields (B = 10 12 G). Xi et al (2020) suggest that the compact feature is not a point source and is a knot of ejecta (see Section 4.4 for more details).…”

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confidence: 99%

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The Center of Expansion and Age of the Oxygen-rich Supernova Remnant 1E 0102.2-7219

Banovetz,

Milisavljevic,

Sravan

et al. 2021

Preprint

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We present new proper motion measurements of optically emitting oxygen-rich knots of supernova remnant 1E 0102.2-7219 (E0102), which are used to estimate the remnant's center of expansion and age. Four epochs of high resolution Hubble Space Telescope images spanning 19 yr were retrieved and analyzed. We found a robust center of expansion of α=1 h 04 m 02.48 s and δ=-72 • 01 53.92 (J2000) with 1-σ uncertainty of 1.77 using 45 knots from images obtained with the Advanced Camera for Surveys using the F475W filter in 2003 and 2013 having the highest signal-to-noise ratio. We also estimate an upper limit explosion age of 1738 ± 175 yr by selecting knots with the highest proper motions, that are assumed to be the least decelerated. We find evidence of an asymmetry in the proper motions of the knots as a function of position angle. We conclude that these asymmetries were most likely caused by interaction between E0102's original supernova blast wave and an inhomogeneous surrounding environment, as opposed to intrinsic explosion asymmetry. The observed non-homologous expansion suggests that the use of a free expansion model inaccurately offsets the center of expansion and leads to an overestimated explosion age. We discuss our findings as they compare to previous age and center of expansion estimates of E0102 and their relevance to a recently identified candidate central compact object.

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Section: Proposed Cco Resultsmentioning

confidence: 99%

Section: Proposed Cco Resultsmentioning

confidence: 99%

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confidence: 99%

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The Center of Expansion and Age of the Oxygen-rich Supernova Remnant 1E 0102.2-7219

Banovetz,

Milisavljevic,

Sravan

et al. 2021

Preprint

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“…First, its X-ray spectrum is thermal, ★ E-mail: pshternin@gmail.com shows little or no pulsations and can be described by the emission from the whole NS surface if a carbon atmosphere is assumed (Ho & Heinke 2009; see also Chang, Bildsten & Arras 2010;Wĳngaarden et al 2019). It was the first NS for which the carbon atmosphere model had been successfully applied; several more such sources are known now (see, e.g., Klochkov et al 2013Klochkov et al , 2016Doroshenko et al 2018;Hebbar et al 2020;Ho et al 2021). Second, the star probably shows real-time cooling, much faster than expected from the standard NS cooling models.…”

Section: Introductionmentioning

confidence: 99%

Model-independent constraints on superfluidity from the cooling neutron star in Cassiopeia A

Shternin,

Ofengeim,

et al. 2021

Preprint

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We present a new model-independent (applicable for a broad range of equations of state) analysis of the neutrino emissivity due to triplet neutron pairing in neutron star cores. We find that the integrated neutrino luminosity of the Cooper Pair Formation (CPF) process can be written as a product of two factors. The first factor depends on the neutron star mass, radius and maximal critical temperature of neutron pairing in the core, 𝑇 𝐶𝑛max , but not on the particular superfluidity model; it can be expressed by an analytical formula valid for many nucleon equations of state. The second factor depends on the shape of the critical temperature profile within the star, the ratio of the temperature 𝑇 to 𝑇 𝐶𝑛max , but not on the maximal critical temperature itself. While this second factor depends on the superfluidity model, it obeys several model-independent constraints. This property allows one to analyse the thermal evolution of neutron stars with superfluid cores without relying on a specific model of their interiors. The constructed expressions allow us to perform a self-consistent analysis of spectral data and neutron star cooling theory. We apply these findings to the cooling neutron star in the Cassiopeia A supernova remnant using 14 sets of observations taken over 19 years. We constrain 𝑇 𝐶𝑛max to the range of (5 − 10) × 10 8 K. This value depends weakly on the equation of state and superfluidity model, and will not change much if cooling is slower than the current data suggest. We also constrain the overall efficiency of the CPF neutrino luminosity.

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“…Near the geometric center of Cas A exists an X-ray point source that is likely the NS produced by the SN of Cas A (Tananbaum 1999;Chakrabarty et al 2001), and E0102 may also have a NS within its boundary albeit at an off-center position (Vogt et al 2018). While the NS in E0102 is confirmed by Hebbar et al (2020), it is also challenged by Long et al (2020), who suggest that the X-ray source is an ejecta knot rather than a NS. Within Cas A, fast hydrogen-rich knots were detected to have velocities ∼ 6000 km s −1 , implying condensations from the progenitor's outer layers (Fesen et al 1988;Fesen & Becker 1991), and in E0102 a small amount of fast-moving hydrogen-rich ejecta material is observed to have velocities up to 1785 km s −1 (Seitenzahl et al 2018).…”

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confidence: 99%

Searching for Surviving Companion in the Young SMC Supernova Remnant 1E 0102.2-7219

Li,

Seitenzahl,

Ishioka

et al. 2021

Preprint

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1E 0102.2-7219 (hereafter E0102) is a young supernova remnant (SNR) in the Small Magellanic Cloud (SMC). It contains oxygen-rich SN ejecta, a possible neutron star (NS), and a small amount of fast-moving H-rich ejecta material. These properties are also seen in Cas A, it has thus been suggested that E0102 is also a Type IIb SNR, whose SN progenitor's hydrogen envelope was stripped off possibly via interactions with a companion star. To search for a surviving companion of E0102's SN progenitor, we have used archival Hubble Space Telescope (HST) continuum images to make photometric measurements of stars projected in the SNR to construct color-magnitude diagrams and compare the stars with those expected from surviving companions of Type IIb SNe. We have also used the Multi-Unit Spectroscopic Explorer observations taken with the Very Large Telescope to perform spectroscopic analyses of stars and search for peculiar radial velocities as diagnostics of surviving companions. We further use the HST and Gaia data to inspect proper motions of stars for complementary kinetic studies. No plausible companion candidates are found if the SN explosion site was near the NS, while the B3 V star 34a may be a plausible companion candidate if the SN explosion site is near the SN ejecta's expansion center. If the NS is real and associated with E0102, it needs a ∼1000 km s −1 runaway velocity, which has been observed in other SNRs and can be acquired from an asymmetric SN explosion or a kick by the SN explosion of a massive companion.

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X-ray spectral analysis of the neutron star in SNR 1E 0102.2−7219

Cited by 17 publications

References 92 publications

The Center of Expansion and Age of the Oxygen-rich Supernova Remnant 1E 0102.2-7219

The Center of Expansion and Age of the Oxygen-rich Supernova Remnant 1E 0102.2-7219

Model-independent constraints on superfluidity from the cooling neutron star in Cassiopeia A

Searching for Surviving Companion in the Young SMC Supernova Remnant 1E 0102.2-7219

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