Copyright © Philip M. Parker, INSEAD. Terms of Use.
| Domain | Definition |
Aerospace | A thermonuclear reaction in which two protons collide at very high velocities and combine to form a deuteron. The resultant deuteron may capture another proton to form tritium and the latter may undergo proton capture to form helium. Compare carbon cycle.The proton-proton reaction is now believed to be the principal source of energy within the sun and other stars of its class. A temperature of the order of 5 million degrees Kelvin and high hydrogen (proton) concentrations are required for this reaction to proceed at rates compatible with energy emission by such stars. (references) |
Source: compiled by the editor from various references; see credits. | |
Hexadecimal (or equivalents, 770AD-1900s) (references)50 52 4F 54 4F 4E 2D 50 52 4F 54 4F 4E 52 45 41 43 54 49 4F 4E |
| Leonardo da Vinci (1452-1519; backwards) (references)
|
Binary Code (1918-1938, probably earlier) (references)01010000 01010010 01001111 01010100 01001111 01001110 00101101 01010000 01010010 01001111 01010100 01001111 01001110 00100000 01010010 01000101 01000001 01000011 01010100 01001001 01001111 01001110 |
HTML Code (1990) (references)P R O T O N - P R O T O N   R E A C T I O N |
ISO 10646 (1991-1993) (references)0050 0052 004F 0054 004F 004E 002D 0050 0052 004F 0054 004F 004E 0052 0045 0041 0043 0054 0049 004F 004E |
Encryption (beginner's substitution cypher): (references)5052495449481550524954494825239353754434948 |
| 1. Orthography 2. Bibliography |
Copyright © Philip M. Parker, INSEAD. Terms of Use.
