Description of names and Acronyms in output files
Note: MAPPINGSIII has been developed over two decades by many people. The variations in naming convention and units reflect this. Work is currently underway to introduce more consistency to the Mappings output naming convention.
| ABN | Abundance |
| Accuracy | This parameter reflects the reliability of the atomic data used to estimate the emission-line fluxes. |
| 1 = Accurate to 10% (Hydrogenic lines only) | |
| 2 = Average reliability | |
| 3 = Poor reliability (old data, many atomic levels, or radiative transfer problems | |
| Alpha | Power law model index |
| Cut-off | Model cut-off energy (Ryd) |
| De | Electron density (cm-3) |
| DH | Hydrogen density (cm-3) |
| DIend | Distance at end of density bounded models (cm) |
| DISav | Average radius of each shell (cm) |
| DIST.Ave. | Average radius of each shell (cm) |
| DISfin | Final radius of the nebula (cm) |
| DISout | Radius at the outer edge of each shell (cm) |
| DILUav | Average geometric dilution factor. For plane parallel models, DILUav will be 0.5. For spherical models, it will be close to zero |
| DLOsav | Average differential loss between heating and cooling. This should be close to zero if energy has been conserved in the model |
| Dn | Ion density (cm-3) |
| Dnum | Ion density (cm-3) |
| dr | thickness of each shell (cm) |
| dR | thickness of each shell (cm) |
| dTau | Model step-size. Default=0.04 |
| dVol | Nebula volume in each shell (cm3) |
| El.Dens | Electron density (cm-3) |
| FHI | Fraction of HI in each shell of the nebula |
| FHII | Fraction of HII in each shell of the nebula |
| FHXF | Final fraction of HII at the end of the nebula |
| Fill.F. or F.F. | Filling factor |
| Fren | Required final fraction of ionized hydrogen at model end (1%) |
| FQHeI | Flux of He+ ionizing photons(photons s-1 cm-2) |
| FQHeII | Flux of He++ ionizing photons(photons s-1 cm-2) |
| FQHI | Flux of H+ ionizing photons(photons s-1 cm-2) |
| FQtot | Total Flux of ionizing photons(photons s-1 cm-2) |
| Hden | Hydrogen density (cm-3) |
| Hdens | Hydrogen density (cm-3) |
| Ielen | Atomic number of element whose ionized fraction determines the model ending |
| Int./H-beta | Integrated line intensity divided by the intensity of H-beta |
| Jden | Density model chosen by user: c=isochoric, b=isobaric |
| Jeq | Equilibrium model chosen (E is the recommend value) |
| Jgeo | Geometry model chosen by user: s=spherical, p=plane parallel |
| Jpoen | Ionization state of required model ending |
| Ndens | Ion density (cm-3). For solar abundance, Ndens ~ 1.1*Hdens (hydrogen density) |
| nH | Hydrogen density (cm-3) |
| ne | Electron density (cm-3) |
| MOD | model choice: X=external, B=blackbody, P=power law |
| P5 | Photoionization model that is recommended in version IIIr |
| QHDN | Ionization parameter (cm s-1) defined as: ionizing photon flux per unit area/ion density . For solar abundance, the ion density, Ndens ~ 1.1*Hdens (hydrogen density) |
| QHDH | Ionization parameter (cm s-1) defined as: ionizing photon flux per unit area/hydrogen density. Note: the dimensionless ionization parameter is defined as U=QHDH/c, not as QHDN/c |
| QHDNin | Ionization parameter at the inner edge of the nebula as defined in QHDN above (cm s-1) |
| QHDNav | Average ionization parameter as defined in QHDN above(cm s-1) |
| Remp | Initial radius of the nebula (cm) |
| Rmax | Maximum radius of model (cm) |
| Rsou | Source Radius (cm) |
| Ryd | Rydberg (= 912Å or 13.6eV) |
| Run | Model designation entered by user |
| Tauen | Optical depth at model end for optical-depth limited models |
| Not applicable to web-based moels | |
| TauXF | Optical depth at Hydrogen edge (912Å): optically thick if TauXF > 1, optically thin if TauXF < 1 |
| Te | electron temperature (K) |
| Teav/Te Ave. | Average electron temperature (K) |
| Teini | Initial electron temperature (K) |
| Temp | Blackbody model temperature (K) |
| Tend | Temperature at model end (K) |
| Tfinal | Temperature at model end (K) |
| TOTLOSS | Total energy losses + total heating. This should be close to zero if energy has been conserved in the model. |
| Turn-on | Model turn-on energy (Ryd) |
| Z-star | Metallicity of mappings internal stellar atmosphere models |
| Not applicable to web-based models | |
| ZETAef | Alternative (archaic) measure of ionization parameter |
Based on the Mappings online descriptions.
Last modified: Wed Oct 21 2009