65 research outputs found
Progenitor's signatures in Type Ia supernova remnants
The remnants of Type Ia supernovae can provide important clues about their
progenitor-histories. We discuss two well-observed supernova remnants (SNRs)
that are believed to result from a Type Ia SN and use various tools to shed
light on the possible progenitor history. We find that Kepler's SNR is
consistent with a symbiotic binary progenitor consisted of a white dwarf and an
AGB star. Our hydrosimulations can reproduce the observed kinematic and
morphological properties. For Tycho's remnant we use the characteristics of the
X-ray spectrum and the kinematics to show that the ejecta has likely interacted
with dense circumstellar gas.Comment: 4 pages, 9 figures, proceedings for IAU Symposium 281, Padova, July
201
Modeling the interaction of thermonuclear supernova remnants with circumstellar structures: The case of Tycho's supernova remnant
The well-established Type Ia remnant of Tycho's supernova (SN 1572) reveals
discrepant ambient medium density estimates based on either the measured
dynamics or on the X-ray emission properties. This discrepancy can potentially
be solved by assuming that the supernova remnant (SNR) shock initially moved
through a stellar wind bubble, but is currently evolving in the uniform
interstellar medium with a relatively low density.
We investigate this scenario by combining hydrodynamical simulations of the
wind-loss phase and the supernova remnant evolution with a coupled X-ray
emission model, which includes non-equilibrium ionization. For the explosion
models we use the well-known W7 deflagration model and the delayed detonation
model that was previously shown to provide good fits to the X-ray emission of
Tycho's SNR.
Our simulations confirm that a uniform ambient density cannot simultaneously
reproduce the dynamical and X-ray emission properties of Tycho. In contrast,
models that considered that the remnant was evolving in a dense, but small,
wind bubble reproduce reasonably well both the measured X-ray emission spectrum
and the expansion parameter of Tycho's SNR. Finally, we discuss possible mass
loss scenarios in the context of single- and double-degenerate models which
possible could form such a small dense wind bubble.Comment: 12 pages, 7 figures, accepted for publication in MNRA
The Interaction of Type Ia Supernovae with Planetary Nebulae: the Case of Kepler's Supernova Remnant
One of the key methods for determining the unknown nature of Type Ia
supernovae (SNe Ia) is the search for traces of interaction between the SN
ejecta and the circumstellar structures at the resulting supernova remnants
(SNRs Ia). So far, the observables that we receive from well-studied SNRs Ia
cannot be explained self-consistently by any model presented in the literature.
In this study, we suggest that the circumstellar medium (CSM) being observed to
surround several SNRs Ia was mainly shaped by planetary nebulae (PNe) that
originated from one or both progenitor stars. Performing two-dimensional
hydrodynamic simulations, we show that the ambient medium shaped by PNe can
account for several properties of the CSM that have been found to surround SNe
Ia and their remnants. Finally, we model Kepler's SNR considering that the SN
explosion occurred inside a bipolar PN. Our simulations show good agreement
with the observed morphological and kinematic properties of Kepler's SNR. In
particular, our model reproduces the current expansion parameter of Kepler's
SNR, the partial interaction of the remnant with a dense CSM at its northern
region and finally the existence of two opposite protrusions (`ears') at the
equatorial plane of the SNR.Comment: Accepted for publication in Galaxies, 7 page
Detection of optical emission from the supernova remnant G7.7-3.7
We present the first optical study of the supernova remnant (SNR) G7.7-3.7,
with the aim of determining its evolutionary phase since it has been suggested
to be the remnant of SN 386 AD. We obtained narrow-band images in the filters
H + [NII], H, [OIII], [SII] that revealed faint optical emission
in the southern region of the SNR consisting of two filaments elongated in the
east-west direction aligned with the X-ray emitting region of the remnant. The
filaments were seen in H + [NII], [OIII] images and marginally in the
[SII] images, with a non-detection in H. Long-slit spectroscopy of three
regions along one filament revealed large ratios of [SII] / H =
(1.6-2.5), consistent with that expected for a shock-heated SNR. The [SII]
doublet ratio observed in two of the regions implies an upper limit for the
electron density of the gas, with estimates falling below 400 cm and 600
cm in the respective areas. We discuss potential physical mechanisms
that formed the observed optical filaments and we suggest that most likely they
resulted by a collision of the SNR with a dense circumstellar shell lying at
the southern region of the remnant.Comment: 10 pages, 5 figures, accepted in MNRA
Discovery of an optical cocoon tail behind the runaway HD 185806
Studies on the circumstellar structures around evolved stars provide vital
information on the evolution of the parent star and the properties of the local
interstellar medium. In this work, we present the discovery and
characterization of an optical cocoon tail behind the star HD 185806. The
cocoon apex emission is puzzling, as it is detected in the infrared but shows
no signal in the optical wavelength. The H-alpha and [OIII] fluxes of the
nebular structure vary from 2.7 to 8.5x10^{-12} erg s^{-1} cm^ {-2} and from
0.9 to 7.0x10^{-13} erg s^{-1} cm^{-2}, respectively. Through high-resolution
spectroscopy, we derive the spectral type of the star, construct the
position-velocity diagrams of the cocoon tail for the H-alpha, [OIII] and [NII]
emission lines, and determine its velocity in the range of -100 to 40 km s
^{-1} . Furthermore, we use SED fitting and MESA evolutionary models adopting a
distance of 900 pc, and classify HD 185806 as a 1.3 M star, in the transition
phase between the RGB and early AGB stages. Finally, we study the
morpho-kinematic structure of the cocoon tail using the astronomical software
SHAPE. An ellipsoidal structure, with an inclination of 19 degrees with respect
to the plane of sky is found to better reproduce the observed cocoon tail of HD
185806.Comment: Accepted 2022 June 29. Received 2022 June 24; in original form 2022
May 26, 14 pages. Dedicated to V.G. who passed away on 2 Sept. 202
Detection of optical emission from the supernova remnant G7.7–3.7
The work of VD is supported by a grant from NWO graduate programme/GRAPPA-PhD programme. VD also acknowledges support from the LKBF, subsidy no. 19.2.027. JVHS acknowledges support from STFC grant ST/R000824/1. PZ acknowledges the support from the NWO Veni Fellowship, grant no. 639.041.647 and NSFC grant 11590781. SA thanks the support under the grant 5077 financed by IAASARS/NOA. AdB thanks the support from the Spanish Government Ministerio de Ciencia e Innovación through grants PGC-2018-091, 3741-B-C22, and SEV 2015-0548, from the Canarian Agency for Research, Innovation and Information Society (ACIISI) of the Canary Islands Government, and from the European Regional Development Fund (ERDF), under grant with reference ProID2017010115.We present the first optical study of the supernova remnant (SNR) G7.7–3.7, with the aim of determining its evolutionary phase since it has been suggested to be the remnant of SN 386 AD. We obtained narrow-band images in the filters H α + [N ii], H β, [O iii], [S ii] that revealed faint optical emission in the southern region of the SNR consisting of two filaments elongated in the east–west direction aligned with the X-ray emitting region of the remnant. The filaments were seen in H α + [N ii], [O iii] images and marginally in the [S ii] images, with a non-detection in H β. Long-slit spectroscopy of the three regions along one filament revealed large ratios of [S ii]/H α = (1.6–2.5), consistent with that expected for a shock-heated SNR. The [S ii] doublet ratio observed in two of the regions implies an upper limit for the electron density of the gas, with estimates falling below 400 cm−3 and 600 cm−3 in the respective areas. We discuss potential physical mechanisms that formed the observed optical filaments and we suggest that most likely they resulted by a collision of the SNR with a dense circumstellar shell lying at the southern region of the remnant.Publisher PDFPeer reviewe
Rectangular core-collapse supernova remnants: application to Puppis A
Core-collapse supernova remnants are the gaseous nebulae of galactic
interstellar media (ISM) formed after the explosive death of massive stars.
Their morphology and emission properties depend both on the surrounding
circumstellar structure shaped by the stellar wind-ISM interaction of the
progenitor star and on the local conditions of the ambient medium. In the warm
phase of the Galactic plane (n = 1/cm3, T = 8000 K), an organised magnetic
field of strength 7 microG has profound consequences on the morphology of the
wind bubble of massive stars at rest. In this paper we show through 2.5D
magneto-hydrodynamical simulations, in the context of a Wolf-Rayet-evolving 35
Mo star, that it affects the development of its supernova remnant. When the
supernova remnant reaches its middle age (15 to 20 kyr), it adopts a tubular
shape that results from the interaction between the isotropic supernova ejecta
and the anisotropic, magnetised, shocked stellar progenitor bubble into which
the supernova blast wave expands. Our calculations for non-thermal emission,
i.e. radio synchrotron and inverse Compton radiation, reveal that such
supernova remnants can, due to projection effects, appear as rectangular
objects in certain cases. This mechanism for shaping a supernova remnant is
similar to the bipolar and elliptical planetary nebula production by wind-wind
interaction in the low-mass regime of stellar evolution. If such a rectangular
core-collapse supernova remnant is created, the progenitor star must not have
been a runaway star. We propose that such a mechanism is at work in the shaping
of the asymmetric core-collapse supernova remnant Puppis A.Comment: Accepted at MNRA
Supernova Remnants as Clues to Their Progenitors
Supernovae shape the interstellar medium, chemically enrich their host
galaxies, and generate powerful interstellar shocks that drive future
generations of star formation. The shock produced by a supernova event acts as
a type of time machine, probing the mass loss history of the progenitor system
back to ages of 10 000 years before the explosion, whereas supernova
remnants probe a much earlier stage of stellar evolution, interacting with
material expelled during the progenitor's much earlier evolution. In this
chapter we will review how observations of supernova remnants allow us to infer
fundamental properties of the progenitor system. We will provide detailed
examples of how bulk characteristics of a remnant, such as its chemical
composition and dynamics, allow us to infer properties of the progenitor
evolution. In the latter half of this chapter, we will show how this exercise
may be extended from individual objects to SNR as classes of objects, and how
there are clear bifurcations in the dynamics and spectral characteristics of
core collapse and thermonuclear supernova remnants. We will finish the chapter
by touching on recent advances in the modeling of massive stars, and the
implications for observable properties of supernovae and their remnants.Comment: A chapter in "Handbook of Supernovae" edited by Athem W. Alsabti and
Paul Murdin (18 pages, 6 figures
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