اشترك بالحزمة الذهبية واحصل على وصول غير محدود شمرا أكاديميا
تسجيل مستخدم جديدSN 2005ip: A Luminous Type IIn Supernova Emerging from a Dense Circumstellar Medium as Revealed by X-Ray Observations
473
0
0.0
(
0
)
تأليف
Satoru Katsuda
اسأل ChatGPT حول البحث
ﻻ يوجد ملخص باللغة العربية
We report on X-ray spectral evolution of the nearby Type IIn supernova (SN) 2005ip, based on Chandra and Swift observations covering from ~1 to 6 years after the explosion. X-ray spectra in all epochs are well fitted by a thermal emission model with kT > 7 keV. The somewhat high temperature suggests that the X-ray emission mainly arises from the circumstellar medium heated by the forward shock. We find that the spectra taken 2-3 years since the explosion are heavily absorbed N_H ~ 5e22 cm^{-2}, but the absorption gradually decreases to the level of the Galactic absorption N_H ~ 4e20 cm^{-2} at the final epoch. This indicates that the SN went off in a dense circumstellar medium and that the forward shock has overtaken it. The intrinsic X-ray luminosity stays constant until the final epoch when it drops by a factor of ~2. The intrinsic 0.2-10 keV luminosity during the plateau phase is measured to be ~1.5e41 erg/s, ranking SN 2005ip as one of the brightest X-ray SNe. Based on the column density, we derive a lower-limit of a mass-loss rate to be M_dot ~ 0.015 (V_w/100 km/s) M_sun/yr, which roughly agrees with that inferred from the X-ray luminosity, M_dot ~ 0.02 (V_w/100 km/s) M_sun/yr, where V_w is the circumstellar wind speed. Such a high mass-loss rate suggests that the progenitor star had eruptive mass ejections like a luminous blue variable star. The total mass ejected in the eruptive period is estimated to be ~15 M_sun, indicating that the progenitor mass is greater than ~25 M_sun.
قيم البحث
اقرأ أيضاً
X-ray emission is one of the signposts of circumstellar interaction in supernovae (SNe), but until now, it has been observed only in core-collapse SNe. The level of thermal X-ray emission is a direct measure of the density of the circumstellar medium
(CSM), and the absence of X-ray emission from Type Ia SNe has been interpreted as a sign of a very low density CSM. In this paper, we report late-time (500--800 days after discovery) X-ray detections of SN 2012ca in {it Chandra} data. The presence of hydrogen in the initial spectrum led to a classification of Type Ia-CSM, ostensibly making it the first SN~Ia detected with X-rays. Our analysis of the X-ray data favors an asymmetric medium, with a high-density component which supplies the X-ray emission. The data suggest a number density $> 10^8$ cm$^{-3}$ in the higher-density medium, which is consistent with the large observed Balmer decrement if it arises from collisional excitation. This is high compared to most core-collapse SNe, but it may be consistent with densities suggested for some Type IIn or superluminous SNe. If SN 2012ca is a thermonuclear SN, the large CSM density could imply clumps in the wind, or a dense torus or disk, consistent with the single-degenerate channel. A remote possibility for a core-degenerate channel involves a white dwarf merging with the degenerate core of an asymptotic giant branch star shortly before the explosion, leading to a common envelope around the SN.
We present optical and NIR photometry and spectroscopy of SN 2013L for the first four years post-explosion. SN 2013L was a moderately luminous (M$_{r}$ = -19.0) Type IIn supernova (SN) that showed signs of strong shock interaction with the circumstel
lar medium (CSM). The CSM interaction was equal to or stronger to SN 1988Z for the first 200 days and is observed at all epochs after explosion. Optical spectra revealed multi-component hydrogen lines appearing by day 33 and persisting and slowly evolving over the next few years. By day 1509 the H$alpha$ emission was still strong and exhibiting multiple peaks, hinting that the CSM was in a disc or torus around the SN. SN 2013L is part of a growing subset of SNe IIn that shows both strong CSM interaction signatures and the underlying broad lines from the SN ejecta photosphere. The presence of a blue H$alpha$ emission bump and a lack of a red peak does not appear to be due to dust obscuration since an identical profile is seen in Pa$beta$. Instead this suggests a high concentration of material on the near-side of the SN or a disc inclination of roughly edge-on and hints that SN 2013L was part of a massive interactive binary system. Narrow H$alpha$ P-Cygni lines that persist through the entirety of the observations measure a progenitor outflow speed of 80--130 km s$^{-1}$, speeds normally associated with extreme red supergiants, yellow hypergiants, or luminous blue variable winds. This progenitor scenario is also consistent with an inferred progenitor mass-loss rate of 0.3 - 8.0 $times$ 10$^{-3}$ M$_{sun}$ yr$^{-1}$.
In order to understand the contribution of core-collapse supernovae to the dust budget of the early universe, it is important to understand not only the mass of dust that can form in core-collapse supernovae but also the location and rate of dust for
mation. SN 2005ip is of particular interest since dust has been inferred to have formed in both the ejecta and the post-shock region behind the radiative reverse shock. We have collated eight optical archival spectra that span the lifetime of SN 2005ip and we additionally present a new X-shooter optical-near-IR spectrum of SN 2005ip at 4075d post-discovery. Using the Monte Carlo line transfer code DAMOCLES, we have modelled the blueshifted broad and intermediate width H$alpha$, H$beta$ and He I lines from 48d to 4075d post-discovery using an ejecta dust model. We find that dust in the ejecta can account for the asymmetries observed in the broad and intermediate width H$alpha$, H$beta$ and He I line profiles at all epochs and that it is not necessary to invoke post-shock dust formation to explain the blueshifting observed in the intermediate width post-shock lines. Using a Bayesian approach, we have determined the evolution of the ejecta dust mass in SN 2005ip over 10 years presuming an ejecta dust model, with an increasing dust mass from ~10$^{-8}$ M$_{odot}$ at 48d to a current dust mass of $sim$0.1 M$_{odot}$.
The physical characteristics of dust formed in supernovae is poorly known. In this paper, we investigate the extinction properties of dust formed in the type IIn SN 2005ip. The observed light curves of SN 2005ip all exhibit a sudden drop around 50 da
ys after discovery. This has been attributed to dust formation in the dense circumstellar medium. We modeled the intrinsic light curves in six optical bands, adopting a theoretical model for the luminosity evolution of supernovae interacting with their circumstellar material. From the difference between the observed and intrinsic light curves, we calculated extinction curves as a function of time. The total-to-selective extinction ratio, $R_V$, was determined from the extinction in the B and V bands. The resulting extinction, $A_V$, increases monotonically up to about 1 mag, 150 days after discovery. The inferred $R_V$ value also increases slightly with time, but appears constant in the range 4.5--8, beyond 100 days after discovery. The analysis confirms that dust is likely formed in SN 2005ip, starting about two months after explosion. The high value of $R_V$, that is, gray dust, suggests dust properties different from of the Milky Way. While this result hinges on the assumed theoretical intrinsic light curve evolution, it is encouraging that the fitted light curves are as expected for standard ejecta and circumstellar medium density structures.
HST and ground based observations of the Type IIn SN 2010jl are analyzed, including photometry, spectroscopy in the ultraviolet, optical and NIR bands, 26-1128 days after first detection. At maximum the bolometric luminosity was $sim 3times10^{43}$ e
rg/s and even at 850 days exceeds $10^{42}$ erg/s. A NIR excess, dominating after 400 days, probably originates in dust in the circumstellar medium (CSM). The total radiated energy is $> 6.5times10^{50}$ ergs, excluding the dust component. The spectral lines can be separated into one broad component due to electron scattering, and one narrow with expansion velocity $sim 100$ km/s from the CSM. The broad component is initially symmetric around zero velocity but becomes blueshifted after $sim 50$ days, while remaining symmetric about a shifted centroid velocity. Dust absorption in the ejecta is unlikely to explain the line shifts, and we attribute the shift instead to acceleration by the SN radiation. From the optical lines and the X-ray and dust properties, there is strong evidence for large scale asymmetries in the CSM. The ultraviolet lines indicate CNO processing in the progenitor, while the optical shows a number of narrow coronal lines excited by the X-rays. The bolometric light curve is consistent with a radiative shock in an $r^{-2}$ CSM with a mass loss rate of $sim 0.1$ M_sun/yr. The total mass lost is $> 3$ M_sun. These properties are consistent with the SN expanding into a CSM characteristic of an LBV progenitor with a bipolar geometry. The apparent absence of nuclear processing is attributed to a CSM still opaque to electron scattering.
سجل دخول لتتمكن من نشر تعليقات
التعليقات
جاري جلب التعليقات
سجل دخول لتتمكن من متابعة معايير البحث التي قمت باختيارها
