Supernova of 1572, Tycho’s Supernova

Decourchelle, A.

doi:10.1007/978-3-319-21846-5_48

Cited by 9 publications

(4 citation statements)

References 56 publications

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“…A further way to reduce the mass estimate for a given EM int is if not all unshocked material is iron, but lighter elements are also present. Decourchelle (2017) notes that the comparison of iron-L complex and Si-K line images indicates good mixing of the Si and Fe layers synthesised in the supernova. The mass number of Si is half of that of Fe, so if silicon is present, the mass estimate could be significantly reduced.…”

Section: Internal Absorption and Mass In The Unshocked Ejectamentioning

confidence: 94%

Low-frequency Radio Absorption in Tycho’s Supernova Remnant

Arias

Vink

Zhou

et al. 2019

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Tycho's SNR is the remnant of the type Ia supernova explosion SN1572. In this work we present new low-frequency radio observations with the LOFAR Low-Band and High-Band Antennae, centred at 58 MHz and 143 MHz, and with an angular resolution of 41 and 6 respectively. We compare these maps to VLA maps at 327 MHz and 1420 MHz, and detect the effect of low-frequency absorption in some regions of the remnant due to the presence of free electrons along the line-of-sight. We investigate two origins for the low-frequency free-free absorption that we observe: external absorption from foreground, and internal absorption from Tycho's unshocked ejecta. The external absorption could be due to an ionised thin, diffuse cavity surrounding the SNR (although this cavity would need to be very thin to comply with the neutral fraction required to explain the remnant's optical lines), or it could be due to an over-ionised molecular shell in the vicinity of the remnant. We note that possible ionising sources are the X-ray emission from Tycho, its cosmic rays, or radiation from Tycho's progenitor. For the internal absorption, we are limited by our understanding of the spectral behaviour of the region at unabsorbed radio frequencies. However, the observations are suggestive of free-free absorption from unshocked ejecta inside Tycho's reverse shock.

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Section: Internal Absorption and Mass In The Unshocked Ejectamentioning

confidence: 94%

Low-frequency Radio Absorption in Tycho’s Supernova Remnant

Arias

Vink

Zhou

et al. 2019

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“…In Figure 6 we show a histogram of the distribution of the fit of the power-law spectral index Γ, the temperature of the Fe-Nirich plasma kT 1 , the temperature of the N-O-Ne-Mg-Si-S-Ar-Ca-rich plasma kT 2 , and the column density N H . In the majority of the boxes, the fit provided reasonable parameter values, with Γ ∼ 3.1, kT 1 ∼ 6.7, kT 2 ∼ 2.2, and N H ∼ 0.56 (Hwang & Gotthelf 1997;Hwang et al 2002;Decourchelle 2017). Having obtained for each box the best-fit model of the spectrum, we folded them through the IXPE spatial and spectral response functions using the xpobssim Monte Carlo simulation tool from ixpeobssim as a region of interest with 2 × 624 sources.…”

Section: Appendix B Assessment Of Synchrotron Contribution Across Tychomentioning

confidence: 99%

X-Ray Polarimetry Reveals the Magnetic-field Topology on Sub-parsec Scales in Tycho’s Supernova Remnant

Ferrazzoli

Slane

Prokhorov

et al. 2023

ApJ

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Supernova remnants are commonly considered to produce most of the Galactic cosmic rays via diffusive shock acceleration. However, many questions regarding the physical conditions at shock fronts, such as the magnetic-field morphology close to the particle acceleration sites, remain open. Here we report the detection of a localized polarization signal from some synchrotron X-ray emitting regions of Tycho’s supernova remnant made by the Imaging X-ray Polarimetry Explorer. The derived degree of polarization of the X-ray synchrotron emission is 9% ± 2% averaged over the whole remnant, and 12% ± 2% at the rim, higher than the value of polarization of 7%–8% observed in the radio band. In the west region, the degree of polarization is 23% ± 4%. The degree of X-ray polarization in Tycho is higher than for Cassiopeia A, suggesting a more ordered magnetic field or a larger maximum turbulence scale. The measured tangential direction of polarization corresponds to the radial magnetic field, and is consistent with that observed in the radio band. These results are compatible with the expectation of turbulence produced by an anisotropic cascade of a radial magnetic field near the shock, where we derive a magnetic-field amplification factor of 3.4 ± 0.3. The fact that this value is significantly smaller than those expected from acceleration models is indicative of highly anisotropic magnetic-field turbulence, or that the emitting electrons either favor regions of lower turbulence, or accumulate close to where the orientation of the magnetic field is preferentially radially oriented due to hydrodynamical instabilities.

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“…X-ray observations of supernova remnants (SNRs) offer a unique way to address the relevant open questions, as they allow us to measure the composition and distribution of heavy elements that were synthesized during the SN explosion. In fact, recent observational studies of young, luminous Type Ia SNRs, such as Kepler, Tycho, and SN 1006, have provided important insights into the evolution of the explosions of their progenitors (e.g., Vink 2017;Decourchelle 2017;Katsuda 2017, and references therein). In these young his- torical SNRs, however, the central ejecta might not yet have been heated by the reverse shock and thus are invisible in X-rays.…”

Section: Introductionmentioning

confidence: 99%

Element Stratification in the Middle-Aged Type Ia Supernova Remnant G344.7-0.1

Fukushima,

Yamaguchi,

Slane

et al. 2020

Preprint

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Despite their importance, a detailed understanding of Type Ia supernovae (SNe Ia) remains elusive. X-ray measurements of the element distributions in supernova remnants (SNRs) offer important clues for understanding the explosion and nucleosynthesis mechanisms for SNe Ia. However, it is challenging to observe the entire ejecta mass in X-rays for young SNRs, because the central ejecta may not have been heated by the reverse shock yet. Here we present over 200 kilosecond Chandra observations of the Type Ia SNR G344.7-0.1, whose age is old enough for the reverse shock to have reached the SNR center, providing an opportunity to investigate the distribution of the entire ejecta mass. We reveal a clear stratification of heavy elements with a centrally peaked distribution of the Fe ejecta surrounded by intermediate-mass elements (IMEs: Si, S, Ar Ca) with an arc-like structure. The centroid energy of the Fe K emission is marginally lower in the central Fe-rich region than in the outer IME-rich regions, suggesting that the Fe ejecta were shock-heated more recently. These results are consistent with the prediction for standard SN Ia models, where the heavier elements are synthesized in the interior of an exploding white dwarf. We find, however, that the peak location of the Fe K emission is slightly offset to the west with respect to the geometric center of the SNR. This apparent asymmetry is likely due to the inhomogeneous density distribution of the ambient medium, consistent with our radio observations of the ambient molecular and neutral gas.

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Supernova of 1572, Tycho’s Supernova

Cited by 9 publications

References 56 publications

Low-frequency Radio Absorption in Tycho’s Supernova Remnant

Low-frequency Radio Absorption in Tycho’s Supernova Remnant

X-Ray Polarimetry Reveals the Magnetic-field Topology on Sub-parsec Scales in Tycho’s Supernova Remnant

Element Stratification in the Middle-Aged Type Ia Supernova Remnant G344.7-0.1

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