Type Ia Supernovae

By B. Leibundgut. 2000

147 citations recorded by the source corpus.

Summary. Type Ia Supernovae are in many aspects still enigmatic objects. Their observational and theoretical exploration is in full swing, but we still have plenty to learn about these explosions.Recent years have already witnessed a bonanza of supernova observations. The increased samples from dedicated searches have allowed the statistical investigation of Type Ia Supernovae as a class. The observational data on Type Ia Supernovae are very rich, but the uniform picture of a decade ago has been replaced by several correlations which connect the maximum luminosity with light curve shape, color evolution, spectral appearance, and host galaxy morphology. These correlations hold across almost the complete spectrum of Type Ia Supernovae, with a number of notable exceptions. After 150 days past maximum, however, all observed objects show the same decline rate and spectrum.The observational constraints on explosion models are still rather sparse. Global parameters like synthesized nickel mass, total ejecta mass and explosion energetics are within reach in the next few years. These parameters bypass the complicated calculations of explosion models and radiation transport. The bolometric light curves are a handy tool to investigate the overall appearance of Type Ia Supernovae. The nickel masses derived this way show large variations, which combined with the dynamics from line widths, indicate that the brighter events are also coming from more massive objects.The lack of accurate distances and the uncertainty in the correction for absorption are hampering further progress. Improvements in these areas are vital for the detailed comparison of luminosities and the determination of nickel masses. Coverage at near-infrared wavelengths for a statistical sample of Type Ia Supernovae will at least decrease the dependence on the absorption. Some of the most intriguing features of Type Ia Supernovae are best observed at these wavelengths, like the second peak in the light curve, the depression in the J band, and the unblended [Feii] lines in the ashes.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/b9c08e14b488d66dbf0a48de5ea6592c4d278f86

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

On the evolution of rapidly rotating massive white dwarfs towards supernovae or collapses (2005, background): “Observations indicate that more than 70% of SNe Ia are fairly homogeneous, giving similar brightnesses (MNi 0.6 M ) and light-curves, while about 20%...30% are SN 199bg-type (sub-luminous) or SN 1991T-type (over-luminous) (Hillebrandt & Niemeyer 2000; Leibundgut 2000).”
COSMOLOGICAL IMPLICATIONS FROM OBSERVATIONS OF TYPE IA SUPERNOVAE (2001, methodology): “It should also be noted that the systematic differences in the correction methods (Leibundgut 2000a) do not have an effect on this determination but may well be important for the peak magnitudes and distance moduli used in the Hubble diagram.”
Constraints on the progenitor systems of type Ia supernovae (2005, background): “…systems is unsettling, and must be addressed, if we are to have confidence in the cosmological results provided by SNe Ia. Fortunately, during the past decade, a number of observing campaigns (see Leibundgut 2000, for a list) have obtained excellent data sets for a large number of SNe Ia.”
Cosmic distance-duality as a probe of exotic physics and acceleration (2003, background): “ less signiﬁcant since the signal is not seen in the dA(z) data. We now brieﬂy discuss possible origins for our result. These include known systematic eﬀects such as gravitational lensing or evolution[24]. In the case of inﬁnitesimal lightbeams the reciprocityrelationis unaﬀected bylensing, but in r”
Evolution of Stars and Stellar Populations (2005, background): “Different implementations of this correlation between brightness at maximum and light curve shapes do not provide the same correction to the maximum luminosity (for a detailed discussion on this important issue we refer to reviews by [126] and [127]) with offsets of the order of 0.”
Fourteen months of observations of the possible super-Chandrasekhar mass Type Ia Supernova 2009dc (2010, unknown): “We find a decline of 1.47 ± 0.04 mag per 100 d in B, 1.91 ± 0.02 mag per 100 d in V , 2.78 ± 0.03 mag per 100 d in R and 2.87 ± 0.04 mag per 100 d in I. Leibundgut (2000) find typical decay rates for SNe Ia of 1.4 mag per 100 d in B, 2.8 mag per 100 d in V and 4.2 mag per 100 d in I. SN 2009dc…”
An alternative to the cosmological 'concordance model' (2003, background): “However there are systematic differences in the corrections made for the same objects by the two groups (Leibundgut 2000) which raises legitimate concerns about their validity.”