Neon (Ne)
noble-gasGas
Peso atómico estándar
20,1797 uConfiguración electrónica
[He] 2s2 2p6Punto de fusión
-248,59 °CPunto de ebullición
-246,05 °CDensidad
0,8999 kg/m³Estados de oxidación
0Electronegatividad (Pauling)
N/DEnergía de ionización (1.ª)
21,564541 eVAño de descubrimiento
1898Radio atómico
160 pmDetalles
Neon is a noble gas and the second lightest member of group 18. It is monatomic, colorless, and chemically very inert under ordinary conditions because its outer electron shell is closed. In the atmosphere it is present only as a minor constituent, but it is readily recognized by the intense reddish-orange light emitted in low-pressure electrical discharges. Its technological importance rests mainly on this optical behavior and on its cryogenic properties.
Colourless gaseous element of group 18 on the periodic table (noble gases). Neon occurs in the atmosphere, and comprises 0.0018% of the volume of the atmosphere. It has a distinct reddish glow when used in discharge tubes and neon based lamps. It forms almost no chemical compounds. Neon was discovered in 1898 by Sir William Ramsey and M.W. Travers.
The name derives from the Greek neos for "new". It was discovered from its bright orange spectral lines by the Scottish chemist William Ramsay and the English chemist Morris William Travers in 1898 from a liquefied air sample.
Neon was discovered by Sir William Ramsay, a Scottish chemist, and Morris M. Travers, an English chemist, shortly after their discovery of the element krypton in 1898. Like krypton, neon was discovered through the study of liquefied air. Although neon is the fourth most abundant element in the universe, only 0.0018% of the earth's atmosphere is neon.
From the Greek word neos, new. Discovered by Ramsay and Travers in 1898. Neon is a rare gaseous element present in the atmosphere to the extent of 1 part in 65,000 of air. It is obtained by liquefaction of air and separated from the other gases by fractional distillation.
Pure neon is a colorless, odorless, monatomic gas at ordinary temperature and pressure. When cooled below its boiling point it becomes a colorless cryogenic liquid, and at still lower temperature a solid. In a discharge tube it emits a bright red-orange glow from atomic emission lines.
Neon is best known for luminous advertising signs, indicator lamps, and decorative discharge tubes, where low-pressure neon gives a distinctive red-orange emission. Other gases or phosphors are used for many colors often called “neon” in commerce. Neon is also used in some high-voltage indicators, gas lasers such as helium-neon lasers, and specialized cryogenic applications. Liquid neon has a high refrigeration capacity per unit volume, but its cost limits broad use.
The largest use for neon gas is in advertising signs. Neon is also used to make high voltage indicators and is combined with helium to make helium-neon lasers. Liquid neon is used as a cryogenic refrigerant. Neon is highly inert and forms no known compounds, although there is some evidence that it could form a compound with fluorine.
Although neon advertising signs account for the bulk of its use, neon also functions in high-voltage indicators, lightning arrestors, wave meter tubes, and TV tubes. Neon and helium are used in making gas lasers. Liquid neon is now commercially available and is finding important application as an economical cryogenic refrigerant.
Isotopes in Earth/Planetary Science
Neon is subject to stable isotopic fractionation by physical processes, such as exchange between gas, liquid, and solid phases. Small variations in the isotope-amount ratio n(22Ne)/n(20Ne) have been used to examine gas-liquid exchange processes during groundwater recharge (water moving downward from the surface) and discharge [29] M. Ozima, F. A. Podosek. Noble Gas Geochemistry: 2nd Edition, p. 286, Cambridge University Press, Cambridge, UK (2002)., [101] Noble Gases in Geochemistry and Cosmochemistry: Reviews in Mineralogy and Geochemistry, D. Porcelli, C. J. Ballentine, and R. Wieler (Eds.), p. 844, Mineralogical Society of America and the Geochemical Society, Washington, DC (2002)., [102] F. Peeters, U. Beyerle, W. Aeschbach-Hertig, J. Holocher, M. S. Brennwald, R. Kipfer. Geochim. Cosmochim. Acta.67, 587 (2003)..
Isotopes in Geochronology
Some 21Ne and 22Ne form naturally in the Earth’s crust largely by reactions of 18O and 19F in minerals with neutrons and alpha particles emitted from uranium and thorium decay, called nucleogenic neon isotopes [29] M. Ozima, F. A. Podosek. Noble Gas Geochemistry: 2nd Edition, p. 286, Cambridge University Press, Cambridge, UK (2002)., [101] Noble Gases in Geochemistry and Cosmochemistry: Reviews in Mineralogy and Geochemistry, D. Porcelli, C. J. Ballentine, and R. Wieler (Eds.), p. 844, Mineralogical Society of America and the Geochemical Society, Washington, DC (2002).. In addition, neon isotopes can form at the surface of the Earth and in extraterrestrial bodies by cosmic-ray-induced spallation reactions on magnesium, silicon, aluminum, and sodium [103] T. E. Cerling, H. Craig. Annu. Rev. Earth Planet. Sci.22, 273 (1994)., [104] D. Lal, B. Peters. “Cosmic ray produced radioactivity on the earth”, in Cosmic Rays II, K. Sitte (Ed.), Springer-Verlag, New York (1967).. Analyses of all three stable neon isotopes may be used to distinguish these sources from primordial neon. The relative amounts of atmospheric neon and crustal nucleogenic neon isotopes in deep groundwaters and natural gases have been used in studies of solid-water-gas interactions and migration (Fig. IUPAC.10.1). The cosmogenic component is mainly detected in 21Ne and can be used to determine cosmic-ray exposure ages of rock samples, including meteorites exposed during travel through space and boulders exposed by melting of glacial ice (Fig. IUPAC.10.1).
Isotopes in Industry
Masers (Microwave Amplification by Stimulated Emission of Radiation) containing 20Ne have been used to study quantum physics. 21Ne may also play a role in maser studies of quantum physics [106] W. R. Bennett. Phys. Rev.126, 580 (1962)..
Isotopes Used as a Source of Radioactive Isotope(s)
22Ne is used to produce the radioisotope 22Na via the reaction 22Ne (p, n) 22Na [107] R. Policroniades, E. Moreno, A. Varela, G. Murillo, A. Huerta, M. E. Ortiz, E. Chávez. Rev. Mex. Fis. S.54, 46 (2008).. 20Ne has been used to produce the radioisotope 18F via the reaction 20Ne (d, 4He) 18F [107] R. Policroniades, E. Moreno, A. Varela, G. Murillo, A. Huerta, M. E. Ortiz, E. Chávez. Rev. Mex. Fis. S.54, 46 (2008)..
Neon has no stable neutral compounds known under ordinary chemical conditions. Its very high ionization energy and negligible electron affinity make conventional oxidation states chemically inaccessible. Laboratory studies have identified transient ionic or weakly bound species such as NeH⁺ and van der Waals complexes at low temperature or in plasmas, but these are not isolable bulk compounds. Neon clathrate hydrates have been reported only under suitable low-temperature, high-pressure conditions, where neon is physically trapped rather than chemically bonded.
Neon is a very inert element, however, it has been reported to form a compound with fluorine. It is still questionable if true compounds of neon exist, but evidence is mounting in favor of their existence. The ions, Ne+, (NeAr)+, (NeH)+, and (HeNe+) are known from optical and mass spectrometric studies. Neon also forms an unstable hydrate.
See more information at the Neon compound page.
Neon is not toxic and is not chemically reactive in normal use. The main hazards are physical: compressed gas cylinders can rupture if mishandled, and released gas can displace oxygen in confined spaces. Liquid neon and cold equipment can cause cryogenic burns and embrittle some materials. Discharge devices also involve electrical hazards and, in some cases, fragile glass under reduced pressure.
Atmospheric neon is chemically persistent and does not participate significantly in biological or geochemical reactions. It enters the air mainly from primordial atmospheric inventory and minor natural releases from rocks and waters; it is lost only slowly by atmospheric escape processes. Because it is inert, dilute, and nonbioaccumulative, neon has no known essential biological role and little direct ecological activity.
Commercial neon is obtained by fractional distillation of liquefied air, usually as a minor by-product of large oxygen and nitrogen production. Its low atmospheric abundance makes recovery more specialized than for argon, and purification requires separation from helium, hydrogen, and other light gases. Demand is concentrated in signage, electronics, lasers, and niche cryogenic uses. Recycling is possible from closed systems but is uncommon for small lamps and signs, so supply depends strongly on industrial gas infrastructure.
Obtained from production of liquid air as a byproduct of producing liquid oxygen and nitrogen.
Neon is a cosmically abundant light noble gas made chiefly during stellar nucleosynthesis in massive stars, especially through carbon and oxygen burning stages. It is found in the Sun, stellar atmospheres, nebulae, and planetary atmospheres, although its abundance in rocky planets is reduced by volatility and atmospheric loss. Several stable isotopes occur naturally, with ²⁰Ne dominant on Earth.
- The familiar red-orange sign color is produced by neon itself, not by a coating.
- Many commercial “neon” signs of other colors contain argon, mercury vapor, or phosphors instead.
- Neon was discovered through the fractional distillation of liquid air.
- Liquid neon is denser than liquid helium but boils at a much higher temperature.
- Neon has no known stable neutral compound at ambient conditions.
- The name comes from a Greek word meaning “new.”
Imágenes
Propiedades
Físicas
- Radio atómico (empírico)
- 160 pm Comparar Radio atómico (empírico) de todos los elementos →
- Radio covalente
- 58 pm Comparar Radio covalente de todos los elementos →
- Radio de van der Waals
- 154 pm Comparar Radio de van der Waals de todos los elementos →
- Densidad
- 0,8999 kg/m³ Comparar Densidad de todos los elementos →
- Volumen molar
- 0,0168 L/mol
- Fase en CNPT
- Gas Comparar Fase en CNPT de todos los elementos →
- Punto de fusión
- -248,59 °C Comparar Punto de fusión de todos los elementos →
- Punto de ebullición
- -246,05 °C Comparar Punto de ebullición de todos los elementos →
- Capacidad calorífica específica
- 1,03 J/(g·K) Comparar Capacidad calorífica específica de todos los elementos →
- Capacidad calorífica molar
- 20,786 J/(mol·K) Comparar Capacidad calorífica molar de todos los elementos →
- Estructura cristalina
- Cúbica centrada en las caras Comparar Estructura cristalina de todos los elementos →
Químicas
- Electronegatividad (Allen)
- 4,787
- Afinidad electrónica
- -1,2 eV (valor negativo: se predice que el átomo no capta un electrón adicional)
- Energía de ionización (1.ª)
- 21,564541 eV Comparar Energía de ionización (1.ª) de todos los elementos →
- Energía de ionización (2.ª)
- 40,963111 eV Comparar Energía de ionización (2.ª) de todos los elementos →
- Energía de ionización (3.ª)
- 63,423518 eV Comparar Energía de ionización (3.ª) de todos los elementos →
- Energía de ionización (4.ª)
- 97,190335 eV Comparar Energía de ionización (4.ª) de todos los elementos →
- Energía de ionización (5.ª)
- 126,247435 eV Comparar Energía de ionización (5.ª) de todos los elementos →
- Estados de oxidación
- 0 Comparar Estados de oxidación de todos los elementos →
- Electrones de valencia
- 8 Comparar Electrones de valencia de todos los elementos →
- Configuración electrónica
- [He] 2s2 2p6
Termodinámicas
- Punto triple (temperatura)
- -248,59 °C
- Punto triple (presión)
- 4,34e+4 Pa
- Punto crítico (temperatura)
- -228,658 °C
- Punto crítico (presión)
- 2,6786e+6 Pa
- Calor de fusión
- 0,00347204 eV Comparar Calor de fusión de todos los elementos →
- Calor de vaporización
- 0,01772296 eV Comparar Calor de vaporización de todos los elementos →
- Calor de atomización
- 0 eV
Nucleares
- Protones
- 10 Comparar Protones de todos los elementos →
- Neutrones
- 10 Comparar Neutrones de todos los elementos →
- Isótopos conocidos
- 20 Comparar Isótopos conocidos de todos los elementos →
- Isótopos estables
- 3 Comparar Isótopos estables de todos los elementos →
- Isótopo más estable
- Ne-20
- Año de descubrimiento
- 1898
Abundancia
- Abundancia (corteza terrestre)
- 0,005 mg/kg Comparar Abundancia (corteza terrestre) de todos los elementos →
- Abundancia (océano)
- 1,2 × 10−4 mg/L Comparar Abundancia (océano) de todos los elementos →
Estructura cristalina
- Constante de red a
- 443 pm
Estructura electrónica
- Electrones por capa
- 2, 8 Comparar Electrones por capa de todos los elementos →
Identificadores
- Número CAS
- 7440-01-9 Comparar Número CAS de todos los elementos →
- Símbolo del término
- 1S0
- InChI
- InChI=1S/Ne
- Clave InChI
- GKAOGPIIYCISHV-UHFFFAOYSA-N
Configuración electrónica Medido
Ne: 2s² 2p⁶[He] 2s² 2p⁶1s² 2s² 2p⁶Modelo atómico
Los isótopos cambian el número de neutrones, la masa y la estabilidad, pero no la configuración electrónica de un átomo neutro.
Modelo atómico esquemático, no a escala.
Huella atómica
Espectro de emisión / absorción
Distribución isotópica
| Número másico | Masa atómica (u) | Abundancia natural | Periodo de semidesintegración |
|---|---|---|---|
| 20 Estable | 19,9924401762 ± 0,0000000017 | 90,4800% | Estable |
| 21 Estable | 20,993846685 ± 0,000000041 | 0,2700% | Estable |
| 22 Estable | 21,991385114 ± 0,000000018 | 9,2500% | Estable |
Fase / Estado
Motivo: 271,1 °C por encima del punto de ebullición (-246,05 °C)
Esquemático, no a escala
Puntos de transición de fase
Energías de transición
Energía necesaria para fundir 1 mol en el punto de fusión
Energía necesaria para vaporizar 1 mol en el punto de ebullición
Densidad
En condiciones estándar
Estimada mediante la ley de los gases ideales a la T actual
Avanzado
Espectros atómicos
Líneas disponibles ?
| Ion | Carga | Total de líneas | Probabilidades de transición | Designaciones de los niveles |
|---|---|---|---|---|
| Ne I | 0 | 1597 | 533 | 1597 |
| Ne II | +1 | 1914 | 233 | 1912 |
| Ne III | +2 | 910 | 637 | 910 |
| Ne IV | +3 | 643 | 72 | 643 |
| Ne V | +4 | 374 | 139 | 374 |
| Ne VI | +5 | 515 | 449 | 515 |
| Ne VII | +6 | 661 | 442 | 661 |
| Ne VIII | +7 | 745 | 540 | 745 |
| Ne IX | +8 | 229 | 228 | 229 |
| Ne X | +9 | 137 | 137 | 137 |
Niveles disponibles ?
| Ion | Carga | Niveles |
|---|---|---|
| Ne I | 0 | 375 |
| Ne II | +1 | 385 |
| Ne III | +2 | 283 |
| Ne IV | +3 | 215 |
| Ne V | +4 | 161 |
| Ne VI | +5 | 135 |
| Ne VII | +6 | 208 |
| Ne VIII | +7 | 178 |
| Ne IX | +8 | 110 |
| Ne X | +9 | 149 |
Compuestos
Isótopos (3)
Natural neon is a mixture of three isotopes. Six other unstable isotopes are known.
| Número másico | Masa atómica (u) | Abundancia natural | Periodo de semidesintegración | Modo de desintegración | |
|---|---|---|---|---|---|
| 20 Estable | 19,9924401762 ± 0,0000000017 | 90,4800% ± 0,0300% | Estable | stable | |
| 21 Estable | 20,993846685 ± 0,000000041 | 0,2700% ± 0,0100% | Estable | stable | |
| 22 Estable | 21,991385114 ± 0,000000018 | 9,2500% ± 0,0300% | Estable | stable |
Líneas espectrales
Se muestran 50 de 1087. De forma predeterminada, solo se muestran las líneas espectrales con intensidad medida.
| Longitud de onda (nm) | Intensidad | Estado de ionización | Tipo | Transición | Exactitud | Fuente | |
|---|---|---|---|---|---|---|---|
| 692.94673 nm | 100000 | Ne I | emission | 2s2.2p5.(2P*<1/2>).3s 2[1/2]* → 2s2.2p5.(2P*<3/2>).3p 2[3/2] | Medida | NIST | |
| 703.24131 nm | 85000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3s 2[3/2]* → 2s2.2p5.(2P*<3/2>).3p 2[1/2] | Medida | NIST | |
| 717.39381 nm | 77000 | Ne I | emission | 2s2.2p5.(2P*<1/2>).3s 2[1/2]* → 2s2.2p5.(2P*<3/2>).3p 2[5/2] | Medida | NIST | |
| 724.51666 nm | 77000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3s 2[3/2]* → 2s2.2p5.(2P*<3/2>).3p 2[1/2] | Medida | NIST | |
| 743.88984 nm | 60000 | Ne I | emission | 2s2.2p5.(2P*<1/2>).3s 2[1/2]* → 2s2.2p5.(2P*<3/2>).3p 2[1/2] | Medida | NIST | |
| 702.40504 nm | 34000 | Ne I | emission | 2s2.2p5.(2P*<1/2>).3s 2[1/2]* → 2s2.2p5.(2P*<3/2>).3p 2[3/2] | Medida | NIST | |
| 748.88712 nm | 32000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[1/2] → 2s2.2p5.(2P*<3/2>).3d 2[3/2]* | Medida | NIST | |
| 540.05618 nm | 20000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3s 2[3/2]* → 2s2.2p5.(2P*<1/2>).3p 2[1/2] | Medida | NIST | |
| 585.24879 nm | 20000 | Ne I | emission | 2s2.2p5.(2P*<1/2>).3s 2[1/2]* → 2s2.2p5.(2P*<1/2>).3p 2[1/2] | Medida | NIST | |
| 640.22472 nm | 20000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3s 2[3/2]* → 2s2.2p5.(2P*<3/2>).3p 2[5/2] | Medida | NIST | |
| 470.43948 nm | 15000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[1/2] → 2s2.2p5.(2P*<3/2>).5d 2[3/2]* | Medida | NIST | |
| 471.20625 nm | 15000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[5/2] → 2s2.2p5.(2P*<3/2>).6d 2[5/2]* | Medida | NIST | |
| 471.53441 nm | 15000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[5/2] → 2s2.2p5.(2P*<3/2>).6d 2[7/2]* | Medida | NIST | |
| 650.65281 nm | 15000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3s 2[3/2]* → 2s2.2p5.(2P*<3/2>).3p 2[5/2] | Medida | NIST | |
| 470.88584 nm | 12000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[1/2] → 2s2.2p5.(2P*<3/2>).5d 2[1/2]* | Medida | NIST | |
| 453.77551 nm | 10000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[1/2] → 2s2.2p5.(2P*<1/2>).5d 2[3/2]* | Medida | NIST | |
| 471.00638 nm | 10000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[1/2] → 2s2.2p5.(2P*<3/2>).5d 2[1/2]* | Medida | NIST | |
| 478.89249 nm | 10000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[5/2] → 2s2.2p5.(2P*<3/2>).7s 2[3/2]* | Medida | NIST | |
| 482.73382 nm | 10000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[1/2] → 2s2.2p5.(2P*<3/2>).6s 2[3/2]* | Medida | NIST | |
| 488.49181 nm | 10000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[5/2] → 2s2.2p5.(2P*<1/2>).5d 2[5/2]* | Medida | NIST | |
| 495.70324 nm | 10000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[3/2] → 2s2.2p5.(2P*<1/2>).5d 2[5/2]* | Medida | NIST | |
| 534.10932 nm | 10000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[1/2] → 2s2.2p5.(2P*<3/2>).4d 2[1/2]* | Medida | NIST | |
| 588.18952 nm | 10000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3s 2[3/2]* → 2s2.2p5.(2P*<1/2>).3p 2[1/2] | Medida | NIST | |
| 602.99969 nm | 10000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3s 2[3/2]* → 2s2.2p5.(2P*<1/2>).3p 2[1/2] | Medida | NIST | |
| 607.43377 nm | 10000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3s 2[3/2]* → 2s2.2p5.(2P*<3/2>).3p 2[1/2] | Medida | NIST | |
| 614.30626 nm | 10000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3s 2[3/2]* → 2s2.2p5.(2P*<3/2>).3p 2[3/2] | Medida | NIST | |
| 616.35939 nm | 10000 | Ne I | emission | 2s2.2p5.(2P*<1/2>).3s 2[1/2]* → 2s2.2p5.(2P*<1/2>).3p 2[1/2] | Medida | NIST | |
| 621.72812 nm | 10000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3s 2[3/2]* → 2s2.2p5.(2P*<3/2>).3p 2[3/2] | Medida | NIST | |
| 626.6495 nm | 10000 | Ne I | emission | 2s2.2p5.(2P*<1/2>).3s 2[1/2]* → 2s2.2p5.(2P*<1/2>).3p 2[3/2] | Medida | NIST | |
| 633.44278 nm | 10000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3s 2[3/2]* → 2s2.2p5.(2P*<3/2>).3p 2[5/2] | Medida | NIST | |
| 638.29917 nm | 10000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3s 2[3/2]* → 2s2.2p5.(2P*<3/2>).3p 2[3/2] | Medida | NIST | |
| 659.89529 nm | 10000 | Ne I | emission | 2s2.2p5.(2P*<1/2>).3s 2[1/2]* → 2s2.2p5.(2P*<1/2>).3p 2[1/2] | Medida | NIST | |
| 705.91074 nm | 10000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[1/2] → 2s2.2p5.(2P*<1/2>).3d 2[3/2]* | Medida | NIST | |
| 576.44189 nm | 7000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[5/2] → 2s2.2p5.(2P*<3/2>).4d 2[7/2]* | Medida | NIST | |
| 533.07771 nm | 6000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[1/2] → 2s2.2p5.(2P*<3/2>).4d 2[3/2]* | Medida | NIST | |
| 534.3282 nm | 6000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[1/2] → 2s2.2p5.(2P*<3/2>).4d 2[1/2]* | Medida | NIST | |
| 597.5534 nm | 6000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3s 2[3/2]* → 2s2.2p5.(2P*<1/2>).3p 2[3/2] | Medida | NIST | |
| 475.27311 nm | 5000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[5/2] → 2s2.2p5.(2P*<3/2>).6d 2[7/2]* | Medida | NIST | |
| 479.02171 nm | 5000 | Ne I | emission | 2s2.2p5.(2P*<1/2>).3p 2[3/2] → 2s2.2p5.(2P*<1/2>).6d 2[5/2]* | Medida | NIST | |
| 483.73128 nm | 5000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[1/2] → 2s2.2p5.(2P*<3/2>).6s 2[3/2]* | Medida | NIST | |
| 489.20896 nm | 5000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[3/2] → 2s2.2p5.(2P*<3/2>).7s 2[3/2]* | Medida | NIST | |
| 500.51582 nm | 5000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[3/2] → 2s2.2p5.(2P*<1/2>).5d 2[5/2]* | Medida | NIST | |
| 503.77504 nm | 5000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[5/2] → 2s2.2p5.(2P*<3/2>).5d 2[7/2]* | Medida | NIST | |
| 514.49371 nm | 5000 | Ne I | emission | 2s2.2p5.(2P*<1/2>).3p 2[3/2] → 2s2.2p5.(2P*<1/2>).5d 2[5/2]* | Medida | NIST | |
| 514.50308 nm | 5000 | Ne I | emission | 2s2.2p5.(2P*<1/2>).3p 2[3/2] → 2s2.2p5.(2P*<1/2>).5d 2[5/2]* | Medida | NIST | |
| 556.27668 nm | 5000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[5/2] → 2s2.2p5.(2P*<1/2>).4d 2[5/2]* | Medida | NIST | |
| 565.66578 nm | 5000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[3/2] → 2s2.2p5.(2P*<1/2>).4d 2[5/2]* | Medida | NIST | |
| 571.92256 nm | 5000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[3/2] → 2s2.2p5.(2P*<1/2>).4d 2[5/2]* | Medida | NIST | |
| 574.82979 nm | 5000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[5/2] → 2s2.2p5.(2P*<3/2>).4d 2[5/2]* | Medida | NIST | |
| 580.44496 nm | 5000 | Ne I | emission | 2s2.2p5.(2P*<3/2>).3p 2[5/2] → 2s2.2p5.(2P*<3/2>).4d 2[5/2]* | Medida | NIST |
Propiedades ampliadas
Radios covalentes (ampliados)
- Radio covalente (Pyykkö)
- 67 pm
- Radio covalente (Pyykkö, enlace doble)
- 96 pm
Radios de van der Waals
- Bondi
- 154 pm
- Alvarez
- 158 pm
- UFF
- 324,3 pm
- MM3
- 160 pm
Radios atómicos y metálicos
- Radio atómico (Rahm)
- 156 pm
Escalas de numeración
- Mendeleev
- 113
- Pettifor
- 2
- Glawe
- 2
Escalas de electronegatividad
- Ghosh
- 0
- Gunnarsson–Lundqvist
- 7
- Robles–Bartolotti
- 7
Polarizabilidad y dispersión
- Polarizabilidad dipolar
- 2,6611 a.u.
- Polarizabilidad dipolar (incert.)
- 0 a.u.
- C₆
- 6,2 Ha·Bohr6
- C₆ (Gould–Bučko)
- 6,91 Ha·Bohr6
Afinidad química
- Afinidad protónica
- 198,8 kJ/mol
- Basicidad en fase gaseosa
- 174,4 kJ/mol
Propiedades de los gases nobles
Transiciones de fase y alótropos
| Punto de fusión | 24,56 K |
| Punto de ebullición | 27,1 K |
| Punto crítico (temperatura) | 44,49 K |
| Punto crítico (presión) | 2,68 MPa |
| Punto triple (temperatura) | 24,56 K |
| Punto triple (presión) | 43,37 kPa |
Datos de referencia avanzados
Constantes de apantallamiento (3)
| n | Orbital | σ |
|---|---|---|
| 1 | s | 0,3579 |
| 2 | p | 4,2416 |
| 2 | s | 4,2416 |
Modos de desintegración de los isótopos (35)
| Isótopo | Modo | Intensidad |
|---|---|---|
| 15 | 2p | 100% |
| 16 | 2p | 100% |
| 17 | B+ | 100% |
| 17 | B+p | 94,4% |
| 17 | B+A | 3,5% |
| 17 | B+pA | 0% |
| 18 | B+ | 100% |
| 19 | B+ | 100% |
| 23 | B- | 100% |
| 24 | B- | 100% |
Factores de dispersión de rayos X (503)
| Energía (eV) | f₁ | f₂ |
|---|---|---|
| 10 | — | 0 |
| 10,1617 | — | 0 |
| 10,3261 | — | 0 |
| 10,4931 | — | 0 |
| 10,6628 | — | 0 |
| 10,8353 | — | 0 |
| 11,0106 | — | 0 |
| 11,1886 | — | 0 |
| 11,3696 | — | 0 |
| 11,5535 | — | 0 |
Datos adicionales
Estimated Crustal Abundance
The estimated element abundance in the earth's crust.
5×10-3 milligrams per kilogram
Referencias (1)
Estimated Oceanic Abundance
The estimated element abundance in the earth's oceans.
1.2×10-4 milligrams per liter
Referencias (1)
Referencias
(9)
Data deposited in or computed by PubChem
The half-life and atomic mass data was provided by the Atomic Mass Data Center at the International Atomic Energy Agency.
Element data are cited from the Atomic weights of the elements (an IUPAC Technical Report). The IUPAC periodic table of elements can be found at https://iupac.org/what-we-do/periodic-table-of-elements/. Additional information can be found within IUPAC publication doi:10.1515/pac-2015-0703 Copyright © 2020 International Union of Pure and Applied Chemistry.
The information are cited from Pure Appl. Chem. 2018; 90(12): 1833-2092, https://doi.org/10.1515/pac-2015-0703.
Thomas Jefferson National Accelerator Facility (Jefferson Lab) is one of 17 national laboratories funded by the U.S. Department of Energy. The lab's primary mission is to conduct basic research of the atom's nucleus using the lab's unique particle accelerator, known as the Continuous Electron Beam Accelerator Facility (CEBAF). For more information visit https://www.jlab.org/
The periodic table at the LANL (Los Alamos National Laboratory) contains basic element information together with the history, source, properties, use, handling and more. The provenance data may be found from the link under the source name.
The periodic table contains NIST's critically-evaluated data on atomic properties of the elements. The provenance data that include data for atomic spectroscopy, X-ray and gamma ray, radiation dosimetry, nuclear physics, and condensed matter physics may be found from the link under the source name. Ref: https://www.nist.gov/pml/atomic-spectra-database
This section provides all form of data related to element Neon.
The element property data was retrieved from publications.