By Regina von Berlepsch
ISBN-10: 3527411135
ISBN-13: 9783527411139
ISBN-10: 3527644385
ISBN-13: 9783527644384
This 23nd quantity within the sequence includes 15 invited experiences provided in the course of the convention AG2010: "Zooming in, the cosmos at excessive resolution"Content:
Read or Download Reviews in Modern Astronomy: Zooming in: The Cosmos at High Resolution, Volume 23 PDF
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Additional info for Reviews in Modern Astronomy: Zooming in: The Cosmos at High Resolution, Volume 23
Sample text
Stellar forensics with the supernova-GRB connection 29 Using our reliable and early-time measurements of the bolometric output of this SN in conjunction with models by Waxman et al. 7 R and 12±7 R , respectively, the latter being more in line with typical WN stars. We furthermore showed that the observed X-ray emission by which it was discovered (Soderberg et al. 2008) is different from those of X-ray flashes, the weaker cousins of GRBs, which demonstrates that even normal SN Ib, surprisingly, can give rise to high-energy phenomena (but see Mazzali et al.
2-m telescope. JHKs data (filled stars, triangles, and squares) are from PAIRITEL. 71 d) from PAIRITEL, amongst the earliest data of a SN Ib to date. Swift/UVOT upper limits are indicated by the arrows. 2-m CfA and the PAIRITEL data (left part). The data have not been corrected for extinction. The two-component light curve is pronounced in the blue, where the 1st peak is due to thermal emission from the expanding and cooling stellar layers and the 2nd peak due to powering by 56 Ni. We note that our earliest ground-based data points are consistent with the light-curve fits by Soderberg et al.
This problem is somewhat more serious in CTTS than in other objects, because of the enhanced Ne abundance often found in CTTS. For a few active MS stars Testa et al. (2004) extrapolated the strength of the higher order Ne X lines from the lower ones, which can be easily measured. They then fit the Mg XI triplet, taking the line blends into account. Brickhouse et al. (2010) analyzed their Chandra/HETGS observations and found that the blending is not important in this case. For densities < 1015 cm−3 the collision time is much longer than the radiative decay time in the Lyman series, thus all excited states decay radiatively and the relative strength of the unabsorbed Ne X lines depends only on the temperature and the collision strength.
Reviews in Modern Astronomy: Zooming in: The Cosmos at High Resolution, Volume 23 by Regina von Berlepsch
by Ronald
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