Am 24. Mai 2017 werde ich beim Arbeitskreis Astronomie im Studium Generale der Universität Stuttgart einen öffentlichen Abendvortrag über Typ Ia Supernovae halten. Der Vortrag beginnt um 19:30 im Hörsaal V 31.01 auf dem Campus Vaihingen.
Kurzzusammenfassung: In den Endphasen ihrer Entwicklung durchlaufen Sterne dramatische Prozesse die zu gewaltigen Explosionen führen. Diese sogenannten Supernovae spielen eine wichtige Rolle für die chemische Entwicklung des Universums und lassen sich auf Grund ihrer immensen Helligkeit auch noch in entfernten Galaxien beobachten. Eine bestimmte Klasse von Supernovae hat in den letzten zwei Jahrzehnten besondere Aufmerksamkeit erfahren. Eine empirische Relation zwischen der Helligkeit und zeitlichen Entwicklung dieser Typ Ia Supernovae macht sie zu kosmischen Leuchtfeuern, mit denen sich grosse Entfernungen im Universum vermessen lassen. Ende der 1990er Jahre hat die Anwendung dieses Verfahrens zu einer Revolution in unserem Verständnis vom Universum geführt. Bei der Vermessung weit entfernter Typ Ia Supernovae stellte sich heraus, dass diese dunkler waren als im Rahmen des damaligen kosmologischen Standardmodells erwartet wurde. Dies lässt sich nur dadurch erklären, dass unser Universum beschleunigt expandiert. Trotz dieser enormen Bedeutung für die moderne Astrophysik ist der Explosionsmechanismus von Typ Ia Supernovae und die Frage nach ihren Vorläufersternen immer noch nicht vollständig geklärt. In diesem Vortrag werde ich aktuelle Beobachtungsergebnisse und neue Computersimulationen zu Typ Ia Supernovae vorstellen, die dazu beitragen unser Verständnis dieser kosmischen Leuchtfeuer zu verbessern.
On March 27-31 an international astrophysics conference on the AGB-Supernovae mass transition was held at the Observatory of Rome in Frascati, Italy. About 100 researchers from all over the world discussed the evolution of stars that start their life with a mass of about 7 to 11 solar masses and reach the super-asymptotic giant branch (AGB) phase during their later evolution. At least three different types of supernovae are connected with the limits of this mass range: isolated stars with an initial mass larger than 11 solar masses end their lives as core collapse supernovae (Type II SN). An initial stellar mass of 7 solar masses is the upper limit for the formation of carbon-oxygen white dwarf stars, whose subsequent evolution through mass transfer in a binary system may lead to thermonuclear supernova explosions (Type Ia SN). Finally, single stars in the super-AGB upper mass range may be the site of electron-capture supernovae. I was invited to provide a review about recent progress in the modelling of Type Ia supernovae on this conference.
After three exciting and stimulating years as an Oskar Klein Fellow at Stockholm University’s Oskar Klein Centre, I am moving to Heidelberg on October 1st to take up a new position as Gliese Fellow at the Zentrum für Astronomie der Universität Heidelberg (ZAH). In close collaboration with scientists from the PSO group at the Heidelberg Institute for Theoretical Studies (HITS) I will use theoretical models to shed light on the progenitors and physical mechanisms of stellar explosions.
I am in Garching to participate in a four week program on the physics of supernovae at the Munich Institute for Astro- and Particle Physics. In the last week of the program there will be a conference on peculiar supernovae, where I am invited to give a review talk on the progenitors of Type Iax supernovae.
Ejecta structure of our GCD model at 60s past explosion. Burning products from the off-centre ignited detonation (indicated by the blue surface) are engulfed by deflagration ashes (shown in red and rendered semi-transparently to allow to see the detonation ashes).
The gravitationally confined detonation (GCD) model has been proposed as a possible explosion mechanism for Type Ia supernovae (SNe) in the single-degenerate evolution channel. Driven by buoyancy, a deflagration flame rises in a narrow cone towards the surface of the exploding white dwarf star. For the most part, the flow of the expanding ashes remains radial, but upon reaching the outer, low-pressure layers of the white dwarf, an additional lateral component develops. This makes the deflagration ashes converge again at the opposite side, where the compression heats fuel and a detonation may be launched. To test the GCD model, we perform a 3D explosion simulation for a model with an ignition spot offset near the upper limit of what is still justifiable, 200 km. This simulation meets our deliberately optimistic detonation criteria and we initiate a detonation. The detonation burns through the white dwarf and leads to its complete disruption. We determine nucleosynthetic yields by post-processing a million tracer particles with a 384 nuclide reaction network and we present multi-band light curves and time-dependent optical spectra. We find that our synthetic observables show a prominent viewing-angle sensitivity in UV and blue bands, which is in tension with observed SNe Ia.
Synthetic spectra of our GCD model at around maximum light. The asymmetry of the ejecta imposes a strong viewing-angle sensitivity at at short wavelengths.
The strong dependence on viewing-angle is caused by the asymmetric distribution of the deflagration ashes in the outer ejecta layers. Finally, we perform a comparison of our model to SN 1991T. The overall flux-level of the model is slightly too low and the model predicts pre-maximum light spectral features due to Ca, S, and Si that are too strong compared SN 1991T. We therefore find it unlikely that the GCD model can explain SN 1991T or similar SNe.
Paper accepted for publication in Astronomy and Astrophysics, full text available at http://arxiv.org/abs/1606.00089
Synthetic spectral time series of our merger model (dark red line) and the observed spectral evolution of iPTF14atg (black line, epochs denote the time since explosion). The light red area indicates the spread due to different viewing angles from the asymmetric merger ejecta.
iPTF14atg, a subluminous peculiar Type Ia supernova (SN Ia) similar to SN 2002es, is the first SN Ia for which a strong UV flash was observed in the early-time light curves. This has been interpreted as evidence for a single-degenerate (SD) progenitor system where such a signal is expected from interactions between the SN ejecta and the non-degenerate companion star. In this paper, we compare synthetic observables of multi-dimensional state-of-the-art explosion models for different progenitor scenarios to the light curves and spectra of iPTF14atg. From our models, we have difficulties explaining the spectral evolution of iPTF14atg within the SD progenitor channel. In contrast, we find that a violent merger of two carbon-oxygen white dwarfs with 0.9 and 0.76 solar masses, respectively, provides an excellent match to the spectral evolution of iPTF14atg from 10d before to several weeks after maximum light. Our merger model does not naturally explain the initial UV flash of iPTF14atg. We discuss several possibilities like interactions of the SN ejecta with the circus-stellar medium and surface radioactivity from a He ignited merger that may be able to account for the early UV emission in violent merger models.
Paper published in Monthly Notices of the Royal Astronomical Society, full text available at http://arxiv.org/abs/1604.05730
Although a theorist by training, I am also involved in observational projects. During my postdoctoral fellowship at MPA, I was part of the Nearby Supernova Factory and performed remote observations with the UH88 telescope on Mauna Kea at Hawaii. Currently, I am involved in the Public ESO Spectroscopic Survey for Transient Objects (PESSTO). PESSTO is granted 90 nights per year on ESO‘s New Technology Telescope (NTT) at La Silla Observatory in the Chilean Andes to follow-up astronomical transients.
Credit: ESO/H. Dahle
Together with two colleagues from ESO and MPA, tonight we are starting a three week observation campaign for PESSTO at La Silla. We will use the EFOSC2 and SOFI spectrographs to obtain optical and near-infrared spectra of recent supernovae that are investigated by the collaboration. In addition, we will also classify new transient candidates, which we obtain from wide-field transient surveys like e.g. the La Silla QUEST survey or photometric alerts from ESA’s Gaia satellite.
The violent merger of two carbon–oxygen white dwarfs has been proposed as a viable progenitor for some Type Ia supernovae. However, it has been argued that the strong ejecta asymmetries produced by this model might be inconsistent with the low degree of polarization typically observed in Type Ia supernova explosions. In this paper, we test this claim by carrying out a spectropolarimetric analysis for the model proposed by Pakmor et al. for an explosion triggered during the merger of a 1.1 and 0.9 M⊙ carbon–oxygen white dwarf binary system. Owing to the asymmetries of the ejecta, the polarization signal varies significantly with viewing angle. We find that polarization levels for observers in the equatorial plane are modest (≲1 per cent) and show clear evidence for a dominant axis, as a consequence of the ejecta symmetry about the orbital plane. In contrast, orientations out of the plane are associated with higher degrees of polarization and departures from a dominant axis.
While the particular model studied here gives a good match to highly polarized events such as SN 2004dt, it has difficulties in reproducing the low polarization levels commonly observed in normal Type Ia supernovae. Specifically, we find that significant asymmetries in the element distribution result in a wealth of strong polarization features that are not observed in the majority of currently available spectropolarimetric data of Type Ia supernovae.
Paper published in Monthly Notices of the Royal Astronomical Society, full text available at http://arxiv.org/abs/1510.04128
On June 25 we hosted a special session “Hunting down the elusive progenitors and explosion mechanisms of Type Ia supernovae” as part of the annual European Week of Astronomy and Space Science which took place on Tenerife (Spain) from June 22-26 .
Our special session aimed at bringing together theorists and observers to give an overview about the current observational state of the art, present recent theoretical progress and discuss the open problems in SNe Ia. The programme consisted of a total of 3 invited talks, 15 contributed talks and 9 posters with participants coming from Australia, Chile, Denmark, Germany, Japan, Netherlands, Russia, Slovakia, Spain, Sweden, Turkey and the United Kingdom. With about 50 scientists attending, the session was quite a success.
The programme was divided in three blocks covering multi-wavelength observations (invited speaker: Assaf Sternberg), binary population synthesis, rates and progenitor searches (invited speaker: Silvia Toonen), and theoretical explosion models and their comparison to observational data (invited speaker: Pablo Loren Aguilar). Highlights of the meeting were presentations on the first gamma-ray detection of a SN Ia, radio constraints on the progenitor of SN 2014J, the discovery of a potential SN Ia progenitor system in a planetary nebula and first synthetic spectropolarimetry for 3D merger models.
Stellar evolution models predict the existence of hybrid white dwarfs (WDs) with a carbon-oxygen core surrounded by an oxygen-neon mantle. Being born with masses ~1.1 Msun, hybrid WDs in a binary system may easily approach the Chandrasekhar mass (MCh) by accretion and give rise to a thermonuclear explosion. In this paper, we investigate an off-centre deflagration in a near-MCh hybrid WD under the assumption that nuclear burning only occurs in carbon-rich material. Performing hydrodynamics simulations of the explosion and detailed nucleosynthesis post-processing calculations, we find that only 0.014 Msun of material is ejected while the remainder of the mass stays bound. The ejecta consist predominantly of iron-group elements, O, C, Si and S.
We also calculate synthetic observables for our model and find reasonable agreement with the faint Type Iax SN 2008ha. This shows for the first time that deflagrations in near-MCh WDs can in principle explain the observed diversity of Type Iax supernovae. Leaving behind a near-MCh bound remnant opens the possibility for recurrent explosions or a subsequent accretion-induced collapse in faint Type Iax SNe, if further accretion episodes occur.
Paper published in Monthly Notices of the Royal Astronomical Society, Volume 450, Issue 3, p.3045-3053, full text available at http://de.arxiv.org/abs/1503.04292
In this paper we present a Monte Carlo radiative transfer technique for calculating synthetic spectropolarimetry for multi-dimensional supernova explosion models. The approach utilises “virtual-packets” that are generated during the propagation of the Monte Carlo quanta and used to compute synthetic observables for specific observer orientations. Compared to extracting synthetic observables by direct binning of emergent Monte Carlo quanta, this virtual-packet approach leads to a substantial reduction in the Monte Carlo noise. This is vital for calculating synthetic spectropolarimetry (since the degree of polarisation is typically very small) but also useful for calculations of light curves and spectra. We first validate our approach via application of an idealised test code to simple geometries. We then describe its implementation in the Monte Carlo radiative transfer code ARTIS and present test calculations for simple models for Type Ia supernovae.
Paper published in Monthly Notices of the Royal Astronomical Society, Volume 450, Issue 1, p.967-981, full text available at http://de.arxiv.org/abs/1503.07002
In this paper we study the very early light curve of supernova 2014J (SN 2014J) using the high-cadence broad-band imaging data obtained by the Kilodegree Extremely Little Telescope (KELT), which fortuitously observed M 82 around the time of the explosion, starting more than two months prior to detection, with up to 20 observations per night. These observations are complemented by observations in two narrow-band filters used in an Hα survey of nearby galaxies by the intermediate Palomar Transient Factory (iPTF) that also captured the first days of the brightening of SN 2014J. Using analytical light curve models, we derive constraints on the progenitor system. The evolution of the light curves is consistent with the expected signal from the cooling of shock heated material at a distance of about a solar radius. This could be due to heated material of the progenitor, a companion star or pre-existing circumstellar environment, e.g., in the form of an accretion disk. Structure seen in the light curves during the first days after explosion could also originate from radioactive material in the outer parts of an exploding white dwarf, as suggested from the early detection of gamma-rays.
Paper published in The Astrophysical Journal, Volume 799, Issue 1, article id. 106, 7 pp. (2015), full text available at http://de.arxiv.org/abs/1410.1363
On September 23/24 2014, I was co-chair of the splinter session Explosive Stellar Transients which was held in the context of the Annual Meeting of the Astronomische Gesellschaft 2014. With 25 oral contributions from various European countries and more than 50 participants our splinter session was a great success.
Detection of a nickel line in the Supernova SN2014J, some two weeks after the explosion. The position of the signal agrees within the measurement error with the position of the supernova (indicated by the cross). Picture from MPE press release.
Type Ia supernovae result from binary systems that include a carbon-oxygen white dwarf, and these thermonuclear explosions typically produce 0.5 solar masses
of radioactive 56Ni. The 56Ni is commonly believed to be buried deeply in the expanding supernova cloud. Surprisingly, in SN2014J we detected the lines at 158 and 812 keV from 56Ni decay (half-life 6.1 days) earlier than the expected several-week time scale, only ~20 days after the explosion, and with flux levels corresponding to roughly 10% of the total expected amount of 56Ni. Some mechanism must break the spherical symmetry of the supernova, and at the same time create a major amount of 56Ni at the outskirts. A plausible explanation is that a belt of helium from the companion star is accreted by the white dwarf, where this material explodes and then triggers the supernova event.
Paper published in Science, Volume 345, Issue 6201, pp. 1162-1165 (2014), full text available at http://de.arxiv.org/abs/1407.3061. Press release at the Max Planck Institute for Extraterrestrial Physics.