Nucleosynthesis in Massive Stars
Nucleosynthesis Data from Woosley & Heger (2007)

Disclaimer:
Note that part of this data is not published in refereed journals and thus may be updated without notice.
We would appreciate if you contact us when using the data on this site for your publications so we may be able to advise you of possbible updates or which data to use..

Run names explained

To uniquely identity the different runs on this page we use our "internal" naming convention rather than that used in various papers. We hope this is not a major inconvenience for you. Please feel free to contact us if you have any question.

The run mames have the following general structure:

s25rA

where

• s is a sentianl for the model initial metallicity; "s" stands for solar composition; a "wr" inidicates that the envelope was removed for selected stars when R > 10¹³ cm.
• 25 gives the mass of the model in solar masses
• r, if present: rerun models with ...
• A is the sential for the supernova explosion "piston" model; variations are in exposion energy and initial mass cut for the piston

Explosion Models:

Explosion Sentinal	Explosion Energy	Initial Pistion Location
A	1.2 B	S = 4
B	2.4 B	S = 4
C	1.2 B	Fe core
D	2.4 B	Fe core

>Discard all below - this page is under constraction; the rest of the page is old stuff

Below we give a brief matrix of model and how there were refenced in publications:

internal name	Rauscher et al. (2002)
s15a28c	S15
s19a28g	S19
s20a28n	S20
s21a28g	S21
s25a28d	S25
s25a28j	S25P
s15a30c	N15
s20a30n	N20
s25a30d	N25
s25a32d	H25

List of the explosion models:

internal name	explosion model / result
s15...c	Ekin = 1.2 foe
s19...g	Ekin = 1.2 foe / 0.1 Msun 56Ni
s20...n	0.1 Msun 56Ni
s21...g	0.1 Msun 56Ni
s25...d	0.1 Msun 56Ni
s25...j	0.2 Msun 56Ni
s30...A s35...A s40...A	Ekin = 1.2 foe
s30...B s35...B s40...B	Ekin = 2.0 foe
s30...C s35...C s40...C	Ekin = 0.6 foe

(Note: 1 foe = ten to the power of fifity-one ergs)

List of reaction rate sets / studies:

internal name	reation rate set	ivspecl
...a27.	RATH + suggested rate for Ne22(a,n) from KAE	2
...a28.	RATH + KAE lower limit Ne22(a,n) rate (HWW)	0
...a29.	RATH + CF88 Ne22(a,n) rate	4
...a30.	RATH + NACRE	1
...a31.	RATH + NACRE with high Ne22(a,n) rate	3
...a32.	HWW coprocessing ("490" isotope network, bdat921)	0
...a33.	RATH + JAE Ne22(a,n) rate	6
...a34.	RATH + JAE Ne22(a,n) high rat	8
...a35.	RATH + JAE Ne22(a,n) low rate	10
...a36.	NACRE + improved fit for high Ne22(a,n) rate	5
...a37.	NACRE + KAE lower limit Ne22(a,n) rate (HWW)	7
...a38.	RATH + JAE Ne22(a,n) rate, but no (a,g)	12
...a39.	RATH + no Ne22(a,n) rate, but KAE low "standard" (a,g)	14
...a40.	RATH + no O16(n,g) (modified bdat file)	0
...a41.	RATH + Fe59(n,g) rate reduced by 2 (modified bdat file)	0

Note:

• RATH = T. Rauscher & F.-K. Thielemann, 2000, At. Data Nucl. Data Tables, 75, 1
• NACRE = C. Angulo et al., Nucl. Phys. A, 656, 3
• HWW = R. D. Hoffman, S. E. Woosley, & T. A. Weaver, 2001, ApJ, 549, 185; rate data
• KAE = F. Käppeler et al., 1994, ApJ, 437, 396
• JAE = M. Jaeger et al., 2001, Phys. Rev. Lett. 87, 202501

Data sets

• (initial) "solar" mass fractions
• Presupernova structure data
• Presupernova composition data
• Postsupernova composition and yield data

Movies

Explosion of Model s25a28d including updated neutrino nucleosynthesis.

content	animated gif	MPEG-1	AVI
bulk	6.9 MByte	4.5 MByte	8.8 MByte
all	21 MByte	18 MByte	30 MByte
radioactivities	5.0 MByte	8.0 MByte	---
19F	4.6 MByte	7.9 MByte	---
g-process	2.5 MByte	4.5 MByte	5.8 MByte
138La	2.3 MByte	4.4 MByte	5.3 MByte
180Ta	2.6 MByte	4.9 MByte	5.8 MByte