astro.wikisort.org - Nebula

A nova remnant is made up of the material either left behind by a sudden explosive fusion eruption by classical novae, or from multiple ejections by recurrent novae. Over their short lifetimes, nova shells show expansion velocities of around 1000 km/s,[1] whose faint nebulosities are usually illuminated by their progenitor stars via light echos as observed with the spherical shell[1] of Nova Persei 1901[2] or the energies remaining in the expanding bubbles like T Pyxidis.[3]

Form

Most novae require a close binary system, with a white dwarf and a main sequence, sub-giant, or red giant star, or the merging of two red dwarfs, so probably all nova remnants must be associated with binaries.[4] This theoretically means these nebula shapes might be affected by their central progenitor stars and the amount of matter ejected by novae.[1] The shapes of these nova nebulae are of much interest to modern astrophysicists.[1][4]

Nova remnants when compared to supernova remnants or planetary nebulae generate much less both in energy and mass. They can be observed for perhaps a few centuries.[1] Notably, more nova remnants have been found with the new novae, due to improved imaging technology like CCD and at other wavelengths. Examples of novae displaying nebula shells or remnants include the following:[1]

• GK Per
• RR Pic
• DQ Her
• FH Ser
• V476 Cyg
• V1974 Cyg
• HR Del
• V1500 Cyg

See also

• Planetary nebula
• Supernova remnant

References

External links

• "T Pyxidis". Hubble Site. Nova Remnant. 1997.
• "Double-star systems cycle between big and small blasts". The Carnegie Observatories. Archived from the original on 8 August 2008.
• "Nova Remnant comparison table". U. Ottawa. Archived from the original on 5 July 2006.
• "Nova Remnant". U. Ottawa. Archived from the original on 5 July 2006.

На других языках

---

- [en] Nova remnant

---

[es] Resto de nova

Un resto de nova es un objeto astronómico formado por el material proveniente de la explosión de una estrella como nova, o por las burbujas de gas expulsadas por una nova recurrente. Su velocidad de expansión es de aproximadamente 1000 km/s, teniendo estos objetos una vida de varios siglos.

---

[ru] Остаток новой

Остаток новой (англ. Nova remnant) — газопылевое образование, состоящее из вещества, оставшегося после вспышки классической новой или после ряда вспышек повторных новых. На протяжении своего существования оболочка новой расширяется со скоростями около 1000 км/с,[1] а туманность подсвечивается световым эхо звезды-предшественника, что наблюдалось в случае сферической оболочки[1] GK Персея[2] и при исследовании энергии, присущей расширяющимся пузырям наподобие T Компаса.[3]

---

---