Japan-Lithuania Opacity Database for Kilonova (version 1.1)

Daiji Kato and Izumi Murakami (National Institute for Fusion Science, Japan)
Masaomi Tanaka and Smaranika Banerjee (Tohoku University, Japan)
Gediminas Gaigalas, Laima Kitovienė, and Pavel Rynkun (Vilnius University, Lithuania)

Numerical data for atomic data and opacities of heavy elements for ejecta of neutron star mergers [1]. The atomic data are calculated using HULLAC (Hebrew University Lawrence Livermore Atomic Code)[2].

M. Tanaka, D. Kato, G. Gaigalas, K. Kawaguchi
“Systematic opacity calculations for kilonovae”
Monthly Notices of the Royal Astronomical Society 496 (2020) 1369-1392.
A. Bar-Shalom, M. Klapisch, J. Oreg
“HULLAC, an integrated computer package for atomic processes in plasmas”
JQSRT 71 (2001) 169-188.

This database is developed by Atomic and Molecular Process Research Section of NIFS in collaboration with Masaomi Tanaka Laboratory of Astronomical Institute in Tohoku University and Computational Atomic Structure Group of Vilnius University. The work was supported by the NINS program for cross-disciplinary science study, the NINS program of Promoting Research by Networking among Institutions (Grant Number 01411702), the Japan Society for the Promotion of Science (JSPS) Bilateral Joint Research Project, and JSPS KAKENHI grant JP19H00694.

In your publications by using our database, please refer to the followings,
D. Kato, I. Murakami, M. Tanaka, S. Banerjee, G. Gaigalas, L. Kitovienė, P. Rynkun, Japan-Lithuania Opacity Database for Kilonova (2021), http://dpc.nifs.ac.jp/DB/Opacity-Database/, (version #.#) and
M. Tanaka, D. Kato, G. Gaigalas, K. Kawaguchi, "Systematic opacity calculations for kilonovae", Monthly Notices of the Royal Astronomical Society 496 (2020) 1369-1392.

Please contact us by email:

Energy level and transition data

readme.txt (information about datafiles)
Download all data (about 600MB)

data available

1st

1
H

2
He

2nd

3
Li

4
Be

5
B

6
C

7
N

8
O

9
F

10
Ne

3rd

11
Na

12
Mg

13
Al

14
Si

15
P

16
S

17
Cl

18
Ar

4th

19
K

20
Ca

21
Sc

22
Ti

23
V

24
Cr

25
Mn

26
Fe

27
Co

28
Ni

29
Cu

30
Zn

31
Ga

32
Ge

33
As

34
Se

35
Br

36
Kr

5th

37
Rb

38
Sr

39
Y

40
Zr

41
Nb

42
Mo

43
Tc

44
Ru

45
Rh

46
Pd

47
Ag

48
Cd

49
In

50
Sn

51
Sb

52
Te

53
I

54
Xe

6th

55
Cs

56
Ba

57-71
La-Lu

72
Hf

73
Ta

74
W

75
Re

76
Os

77
Ir

78
Pt

79
Au

80
Hg

81
Tl

82
Pb

83
Bi

84
Po

85
At

86
Rn

7th

87
Fr

88
Ra

89-103
Ac-Lr

104
Rf

105
Db

106
Sg

107
Bh

108
Hs

109
Mt

110
Ds

111
Rg

112
Cn

113
Nh

114
Fl

115
Mc

116
Lv

117
Ts

118
Og

Lanthanide

57
La

58
Ce

59
Pr

60
Nd

61
Pm

62
Sm

63
Eu

64
Gd

65
Tb

66
Dy

67
Ho

68
Er

69
Tm

70
Yb

71
Lu

Actinide

89
Ac

90
Th

91
Pa

92
U

93
Np

94
Pu

95
Am

96
Cm

97
Bk

98
Cf

99
Es

100
Fm

101
Md

102
No

103
Lr

Planck mean opacity for representative abundance distribution

readme.txt (information about density, temperature, time grids, )
Ye = 0.10, 0.15, 0.20, 0.25, 0.30, 0.35, 0.40

Fig.1: Abundance distribution for diffrent Ye (Wanajo et al. 2014).
fig1

Fig.2: Density dependence of the Planck mean opacity for Ye = 0.25 and t = 1 day. The decline of the opacity at high temperature is due to lack of atomic data for highly ionized ion. This effect is significant for lower density because ionization becomes more efficient (see red curve).
fig2

Fig.3: Temperature and density dependence of the Planck mean opacity for Ye = 0.25 and t = 1 day.
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Version history 1.0: 2021/11/29
Version history 1.1: 2022/12/13

Due to an error in the program, log(gf) values in the energy levels and transition data were not correct in version 1.0.
The error has been corrected, and correct log(gf) values are given in version 1.1.
This error affected only log(gf) values in this database: it does not affect the opacity data nor the results in Tanaka et al. (2020).
We apologize this error. We thank Dr. Andrey Bondarev for pointing out this issue.