CCC-0646 SKYSHINE-KSU.

1. NAME OR DESIGNATION OF PROGRAM:  SKYSHINE-KSU.

3. DESCRIPTION OF PROGRAM OR FUNCTION

This package includes the SKYNEUT 1.1, SKYDOSE 2.2 and MCSKY 2.3 codes plus the DLC-0188/ZZ-SKYDATA library to form a comprehensive system for calculating skyshine doses. SKYNEUT evaluates the neutron and neutron-induced secondary gamma-ray skyshine doses from an isotropic, point, neutron source collimated by three simple geometries: an open silo, a vertical black (perfectly absorbing) wall, and a rectangular building. The source may emit monoenergetic neutrons or neutrons with an arbitrary multigroup spectrum of energies.
SKYDOSE evaluates the gamma-ray skyshine dose from an isotropic, monoenergetic, point gamma-photon source collimated by three simple  geometries: (1) a source in a silo, 2) a source behind an infinitely long, vertical, black wall, and 3) a source in a
rectangular building. In all three geometries an optional overhead slab shield may be specified. MCSKY evaluates the gamma-ray skyshine dose from an isotropic, monoenergetic, point gamma-photon source collimated into either a vertical cone (i.e. silo geometry) or into a vertically oriented structure with an N-sided polygon cross section. An overhead laminate shield composed of two different materials is assumed, although shield thicknesses of zero may be specified to model an unshielded SKYSHINE source.

4. METHOD OF SOLUTION

The SKYNEUT calculation of the skyshine doses uses the integral line-beam method which is based on a newly developed three-parameter approximation of the neutron line-beam response functions.
SKYDOSE is based on the integral line-beam method. For shielded sources, an approximate method is used on exponential attenuation with buildup in the shield.
In MCSKY the skyshine dose calculation is based on a Monte Carlo algorithm to evaluate the gamma-ray transport through the source shields and the integral line-beam method to describe the subsequent transport of gamma photons through the atmosphere.

5. RESTRICTIONS ON THE COMPLEXITY OF THE PROBLEM

For SKYNEUT source neutron energies must be between 0.01 and 14 MeV. For energies above 1 MeV, source-to-detector distances can be as great as 2500 m. For source energies below 1 MeV, the maximum source-to-detector distance is somewhat less. Fluence-to-dose conversion factors are from ICRP Report 51, but *not* include the factor of 2 increase in the neutron quality factor recommended at the 1985 Paris meeting of the ICRP.
For SKYDOSE the source energy E must be between 0.02 and 100 MeV, except for sources with an overhead shield, for which case 0.02 <= E <= 10 MeV. The maximum source-to-detector distance is 3000 m for E <= 10 MeV and 1500 for higher energies.
For MCSKY the source energy may be any energy between 0.02 and 100  MeV. In the Monte Carlo shield calculation, positron transport and bremsstrahlung production are neglected, although the air transport  calculation using the line-beam response function does include these components. Consequently, for heavily shielded sources with energies above about 20 MeV, MCSKY results must be used cautiously especially at detector locations near the source where shield-generated bremsstrahlung may be significant. The maximum source-to-detector distance is 3000 m for E <= 10 MeV and 1500 m for higher source energies.

6. TYPICAL RUNNING TIME

SKYNEUT and SKYDOSE run quickly, requiring only a few seconds per detector location and per source energy group.
The McSKY running time depends primarily on computer speed and number of source particle histories to be followed in the shield, and to a lesser extent on the shield thicknesses and the complexity  of the source collimation.

7. UNUSUAL FEATURES: UNUSUAL FEATURES OF THE PROGRAM

8. RELATED AND AUXILIARY PROGRAMS

DATA LIBRARY: SKYDATA-KSU: Approximate Beam Response Functions
              for Gamma-Ray and Neutron Skyshine Analysis.

10. REFERENCES

- A.A. Gui:
  Response Functions for Neutron Skyshine Analyses, PhD Dissertation       Kansas State University, Manhattan, KS 66506 (1994)
- S.K. Shultis and R.E. Faw:
  Extensions to the Integral Line-Beam Method for Gamma-Ray Skyshine        Analyses
  Report SAND94-2019 (1995)
- J.K. Shultis, R.E. Faw and M.S. Bassett:
  The Integral Line-Beam Method for Gamma Skyshine Analysis
  Nuclear Science Engineering, 107, pp. 228-245 (1991)

- J.K. Shultis, R.E. Faw and F.A. Khan:
  SKYNEUT: A Code for Neutron Skyshine Calculations Using the
  Integral Line-Beam Method
  Report 9503  (Revised January 1997)
- J.K. Shultis, R.E. Faw and C Brockhoff:
  SKYDOSE: A Code for Gamma Skyshine Calculations Using the
  Integral Line-Beam Method
  KSU 9502 (Revised January 1998)
- J.K. Shultis, R.E. Faw and M.H. Stedry:
  McSKY: A Hybrid Monte-Carlo Line-Beam Code for Shielded Gamma
  Skyshine Calculations
  KSU 9501 (Revised October 1997)
- J.K. Shultis, R.E. Faw, A.A. Gui and R.C. Brockhoff:
  Approximate Beam Response Functions for Gamma-Ray and Neutron
  Skyshine Analysis
  Report 271 (June 1995)

11. MACHINE REQUIREMENTS

IBM PC and compatibles. These codes can be easily ported to almost any computer with a FORTRAN 77, 90, 95 compiler.

13. OPERATING SYSTEM UNDER WHICH PROGRAM IS EXECUTED

The codes have been compiled and executed using Lahey F95 and MS DVF under DOS/Windows 98; g77 under Red Hat 6.1 linux; xlf under aix 3.4.

15. NAME AND ESTABLISHMENT OF AUTHORS

Contributed by:
                Radiation Safety Information Computational Center
                Oak Ridge National Laboratory
                Oak Ridge, Tennessee, U. S. A.

Developed by:
                Kansas State University
                Manhattan, Kansas, U.S.A.

README Information file
HIGHGAM.DAT Line-beam response fn E>10 MeV
LOWGAM.DAT Line-beam response fn E<10 MeV
SILO.INP Input file for "silo geometry"
SQUARE.INP Input for "polygon geometry"
SQUARE.DTA Data file needed for SQUARE.INP
MCSKY.FOR Fortran source code
MCSKY.EXE Executable file for DOS machines
SILO.OUT Output produced with SILO.INP data
SQUARE.OUT Output produced with SQUARE.INP
MCSKY.PS Postscript file
MCSKY.PDF File in PDF format
-README Information file
README.DOC Information file
CBGDEI.DAT sec-gamma CBRF DE 10mm ICRU sph.
CBGDEI.TBL sec-gamma CBRF DE 10mm ICRU sph.
CBGDEP.DAT sec-gamma CBRF DE beam ICRU sph.
CBGDEP.TBL sec-gamma CBRF DE beam ICRU sph.
CBGEDE.DAT sec-gamma CBRF EDE anthrop. ph.
CBGEDE.TBL sec-gamma CBRF EDE anthrop. ph.
CBNDEI.DAT n CBRF DE 10mm in the ICRU sph.
CBNDEI.TBL n CBRF DE 10mm in the ICRU sph.
CBNDEP.DAT n CBRF dose - beam on ICRU sph.
CBNDEP.TBL n CBRF dose - beam on ICRU sph.
CBNEDE.DAT n CBRF EDE anthropomorph phantom
CBNEDE.TBL n CBRF EDE anthropomorph phantom
GCFN1.DAT Param. for neutron GCF_n1
GCFN1.TBL Param. for neutron GCF_n1
GCFN2.DAT Param. for neutron GCF_n2
GCFN2.TBL Param. for neutron GCF_n2
GCFSG.DAT Param. for secondary gamma GCF_p
GCFSG.TBL Param. for secondary gamma GCF_p
HIGHGAM.DAT Gamma LBRF E=20 to 100 MeV
LBGDEI.DAT sec-gamma LBRF DE 10mm ICRU sph.
LBGDEI.TBL sec-gamma LBRF DE 10mm ICRU sph.
LBGDEP.DAT sec-gamma LBRF DE beam ICRU sph.
LBGDEP.TBL sec-gamma LBRF DE beam ICRU sph.
LBGEDE.DAT sec-gamma LBRF EDE anthrop. ph.
LBGEDE.TBL sec-gamma LBRF EDE anthrop. ph.
LBNDEI.DAT n LBRF DE 10mm in the ICRU sph.
LBNDEI.TBL n LBRF DE 10mm in the ICRU sph.
LBNDEP.DAT n LBRF dose - beam on ICRU sph.
LBNDEP.TBL n LBRF dose - beam on ICRU sph.
LBNEDE.DAT n LBRF EDE anthropomorph phantom
LBNEDE.TBL n LBRF EDE anthropomorph phantom
LOWGAM.DAT Gamma LBRF E=0.02 to 15 MeV
HIGHGAM.DAT Line-beam response fn E>10 MeV
LOWGAM.DAT Line-beam response fn E<10 MeV
SKYDOSE.FOR Fortran source code
SKYDOSE.EXE Executable for DOS machines
BOX.INP Input file for "box geometry"
-README Information file
SILO.INP Input file for "silo geometry"
SILO.OUT Output produced with SILO.INP data
WALL.INP Input file for "wall geometry"
WALL.OUT Output produced with WALL.INP data
BOX.OUT Output produced with BOX.INP data
SKYDOSE.DOC ASCII version of User's Manual
SKYDOSE.PS Postscript file
SKYDOSE.PDF File in PDF format
GDEP.DAT Param. for secondary gamma LBRF
GEDE.DAT Param. for secondary gamma LBRF
NDEI.DAT Param. for the neutron LBRF
NDEP.DAT Param. for the neutron LBRF
NEDE.DAT Param. for the neutron LBRF
GDEI.DAT Param. for secondary gamma LBRF
SPEC.DAT Data for srce spectrum used by ex.
BOX1.INP Input file for "box geometry" pb 1
BOX2.INP Input file for "box geometry" pb 2
SILO1.INP Input file for "silo geometry"pb1
SILO2.INP Input file for "silo geometry"pb2
WALL2.INP Input file for "wall geometry"pb2
WALL1.INP Input file for "wall geometry"pb1
BOX1.OUT Output produced with BOX1.INP data
BOX2.OUT Output produced with BOX2.INP data
SILO1.OUT Output produced w/SILO1.INP data
SILO2.OUT Output produced w/SILO2.INP data
WALL1.OUT Output produced w/WALL1.INP data
WALL2.OUT Output produced w/WALL2.INP data
-README Information file
SKYNEUT.FOR Fortran source code
SKYNEUT.EXE Executable for DOS machines
SKYNEUT.PS Postscript file
SKYNEUT.PDF File in PDF format