Beam Ion Species and Energies Used Previously at NSRL
 

Ion

Species [1]

Energy [2]

 (MeV/nucleon)

Maximum Intensity [3]

(ions per spill)

LET [4]

(keV/m)

H-1 50 - 2500 6.4 x 1011 1.26 - 0.21
He-4 50 - 1000 0.88 x 1010 5.01 - 0.89
C-12 65 - 1000 1.2 x 1010 36.79 - 8.01
O-16 50 - 1000 0.4 x 1010 80.50 - 14.24
Ne-20 70 - 1000 0.10 x 1010 96.42 - 22.25
Si-28 93 - 1000 0.3 x 1010 151 - 44
Cl-35 500 - 1000 0.2 x 1010 80 - 64
Ar-40 350 0.02 x 1010 105.8
Ti-48 150 - 1000 0.08 x 1010 265 - 108
Fe-56 50 - 1000 0.2 x 1010 832 - 150
Kr-84 383   403
Xe-131 228   1204
Ta-181 292 - 313   1827 - 1896
Au-197 76 - 165 1 x 107 4828 - 3066
Sequential

Field (Fe/H)

1000 Various 150/0.2
Solar Particle Event [5] 30 - 180 Various 1.26 - 0.21

[1] Different isotopes of some ions are also available.  With the commissioning of EBIS, the Electron Beam Ion Source, virtually all ion species will be available.

[2] In general it has become fairly routine to change beam energy, and if a beam energy is not listed in this table, there is not necessarily any reason why it cannot be tuned up at the request of a user.

[3] Intensity per spill refers to the number of ions delivered each spill.  The spill structure during most radiobiology exposures has a 3.8 second repetition time.  During the 3.8 second period, the ions are extracted more or less uniformly in time during a 0.3-0.4 second spill, followed by a ~3.4 second beam-off time.  These intensities were achieved using the Tandem Van De Graaff as the ion source.  When using EBIS, the intensities are significantly lower.

[4] LET, or Linear Energy Transfer is calculated for a water target and is in units of keV per micron.  More detailed LET distributions can be viewed here.

[5] SPE: The August of 1972 solar proton event (SPE) represents one of the largest events on record and the simulated spectra will consists of protons from a few 10ís of MeV to 1 GeV that will approximately represent the Joseph King fit to the observed spectra given by the following equation

Φ(E) = 2.98x108  e-(E-30)/26.5

where E is the proton energy in MeV. The September and October 1989 events represent spectra with larger contributions from high energy protons and will be represented by the integral rigidity spectra

Φ(R)= N e-R/R0

with R0 = 110 MV.

For guidance on expected energy spectra of protons and secondaries behind tissue or other experimental materials including simulation of spacecraft shielding please contact BNL or NASA JSC staff.

NSRL is available to operate blocks of time for SPE simulations in either the standard (20x20 cm2) or a large beam configuration (60x60 cm2). BNL staff will work with approved experiments to facilitate beam sharing during the large beam SPE blocks.

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Last Modified: September 12, 2013
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