All terms in OM

Label Id Description
specific volume SpecificVolume [Specific volume is volume per unit mass.]
angular acceleration AngularAcceleration
electric flux density ElectricFluxDensity
number density NumberDensity
power density PowerDensity
number manual firmness 3.5 NumberManualFirmness3.5 [Firmness manueel: 3.5 = te zacht.]
number manual firmness NumberManualFirmness
admittance Admittance [Admittance is a measure of how easily a circuit or device will allow a current to flow. It is electric current divided by electric potential.]
thermal diffusivity ThermalDiffusivity
straw mass StrawMass
stellar aberration StellarAberration [The apparent angular displacement of the observed position of a celestial object resulting from the motion of the observer. Stellar aberration is divided into diurnal, annual, and secular components.]
aberration Aberration [The apparent angular displacement of the observed position of a celestial object from its geometric position, caused by the finite velocity of light in combination with the motions of the observer and of the observed object.]
stem end rot StemEndRot [Aanwezigheid stem end rot (1/0).]
angular momentum AngularMomentum
magnitude at maximum brightness MagnitudeAtMaximumBrightness [The magnitude at maximum brightness of a variable star.]
magnitude Magnitude [Reverse logarithmic measure of the brightness of an object., The magnitude scale was originally created by Hipparchos of Nicea (160-127 BCE) and was measured by comparing the brightness between stars. Initially this was done inaccurately by eye but is currently done by using photoelectric photometers or even more recently by CCDs. Hipparchos divided the stars into six magnitude (brightness classes), the brightest stars being assigned to the first class and the faintest to the sixth class. By about the middle 1800s it became apparent that the traditional magnitude scale is close to a logarithmic scale with base 2.5. This is due to the fact that the response of the eye is nearly logarithmic. N.R. Pogson formalised the magnitude scale to closely match the traditional (visual) scale. It is now defined as: <math display="block"> <msub><mi>m</mi><mn>1</mn></msub> <mo>-</mo> <msub><mi>m</mi><mn>2</mn> </msub><mo>=</mo> <mn>-2.5</mn><mi>log</mi> <mfrac linethickness="1"> <mrow> <msub><mi>f</mi><mn>1</mn></msub> </mrow> <mrow><msub><mi>f</mi><mn>2</mn></msub> </mrow> </mfrac> </math> where <math display="inline"><msub><mi>m</mi><mn>1</mn></msub> <mo>-</mo> <msub><mi>m</mi><mn>2</mn> </msub></math> is the magnitude difference between two objects, and <math display="inline"><msub><mi>f</mi><mn>1</mn></msub></math> and <math display="inline"><msub><mi>f</mi><mn>2</mn></msub></math> are the luminous fluxes of the two objects. The magnitude of Vega (α Lyrae, HD 172167) is defined to be 0 in all wavelengths and passbands, although in practice this can only be an approximation. The zero point is now defined using multiple standard stars from the north polar sequence (non-variable stars within 2 degrees of the north celestial pole) or secondary standard stars from other parts of the sky. Please note that the scale is inverted, objects of magnitude 1 have a higher luminous flux than objects of magnitude 5. Stars of magnitude 6 are just visible to the naked eye under good observing conditions. The units of magnitude, also called magnitude, are usually not indicated except when indicating small magnitude differences when milli- or micromagnitudes are used.]
moment of force MomentOfForce [Moment of force is the effectiveness of a force to produce rotation about an axis measured by the product of the force and the perpendicular distance from the line of action of the force to the axis.]
Thuan and Gunn magnitude ThuanAndGunnMagnitude [A magnitude measured in one of Thuan and Gunn's standard passbands (using a standard filter, i.e. g).]
prefixed candela PrefixedCandela
prefixed unit PrefixedUnit