Triggers:CNe - Revision history

Lukasz at 15:59, 16 July 2013

2013-07-16T15:59:13Z

Lukasz at 12:02, 23 April 2010

2010-04-23T12:02:22Z

Lukasz at 09:43, 30 March 2010

2010-03-30T09:43:25Z

Lukasz at 11:19, 10 March 2010

2010-03-10T11:19:59Z

Lukasz at 11:13, 10 March 2010

2010-03-10T11:13:11Z

Lukasz at 16:07, 14 December 2009

2009-12-14T16:07:05Z

Lukasz at 16:05, 14 December 2009

2009-12-14T16:05:47Z

Lukasz at 13:46, 28 July 2009

2009-07-28T13:46:29Z

Lukasz: Created page with '* there is roughly 30 novae per year in the Milky Way and about 20 in other galaxies * absolute magnitude $M_V = -8 mag$ * amplitude between 6 and 15 mag * quick rise ...'

2009-07-28T13:38:06Z

Created page with '* there is roughly 30 novae per year in the Milky Way and about 20 in other galaxies * absolute magnitude <math>M_V = -8 mag</math> * amplitude between 6 and 15 mag * quick rise ...'

New page

* there is roughly 30 novae per year in the Milky Way and about 20 in other galaxies
* absolute magnitude <math>M_V = -8 mag</math>
* amplitude between 6 and 15 mag
* quick rise of few days
* slow decline, between few days and 100 days (fast: type A, slow: type B, very slow: type C)
* 15 days after maximum its Mv = -5.5mag, independent on speed or class

@@ Line 2: / Line 2: @@
 (from GCVS).
-* there is roughly 30 novae per year in the Milky Way and about 20 in other galaxies
+* there is observed roughly 10 classical novae per year in the Milky Way and about 40 in other galaxies
 * absolute magnitude <math>M_V = -8 mag</math>
 * spectra near maximum light resemble A-F absorption spectra of luminous stars at first

← Older revision		Revision as of 12:02, 23 April 2010
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	----		----
	Short transient searches in the other galaxies revealed possible new sub-class of novae: [http://uk.arxiv.org/abs/1003.1720 Kasliwal et al. 2010]. They usually stay above the Gaia detection limit for not more than 10 days.		Short transient searches in the other galaxies revealed possible new sub-class of novae: [http://uk.arxiv.org/abs/1003.1720 Kasliwal et al. 2010]. They usually stay above the Gaia detection limit for not more than 10 days.
		+
		+	----
		+	Interesting paper on classification and properties of novae: [[http://uk.arxiv.org/abs/1004.3698 Strope, Schaefer & Henden 2010]]

@@ Line 11: / Line 11: @@
 * 15 days after maximum its Mv = -5.5mag, independent on speed or class
 * small changes at minimum light may be present
 '''Recurrent novae''':

← Older revision		Revision as of 11:19, 10 March 2010
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	----		----
−	Short transient searches in the other galaxies revealed possible new sub-class of novae: [http://uk.arxiv.org/abs/1003.1720 Kasliwal et al. 2010].	+	Short transient searches in the other galaxies revealed possible new sub-class of novae: [http://uk.arxiv.org/abs/1003.1720 Kasliwal et al. 2010]. They usually stay above the Gaia detection limit for not more than 10 days.

← Older revision		Revision as of 11:13, 10 March 2010
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	* example: RS Oph - 3 outbursts between 1957 and 1991 (AAVSO), exhibits some small variation in the baseline in minimum		* example: RS Oph - 3 outbursts between 1957 and 1991 (AAVSO), exhibits some small variation in the baseline in minimum
	* decline within few days		* decline within few days
		+
		+	----
		+	Short transient searches in the other galaxies revealed possible new sub-class of novae: [http://uk.arxiv.org/abs/1003.1720 Kasliwal et al. 2010].

@@ Line 1: / Line 1: @@
-Close binary systems with orbital periods from 0.05 to 230 days. One of the components of these systems is a hot dwarf star that suddenly, during a time interval from one to several dozen or several hundred days, increases its brightness by 7-19 mag in V, then returns gradually to its former brightness over several months, years, or decades. Cool components may be giants, subgiants, or dwarfs of K-M type (from GCVS).
+Close binary systems with orbital periods from 0.05 to 230 days. One of the components of these systems is a hot dwarf star that suddenly, during a time interval from one to several dozen or several hundred days, increases its brightness by 7-19 mag in V, then returns gradually to its former brightness over several months, years, or decades. Cool components may be giants, subgiants, or dwarfs of K-M type
 * there is roughly 30 novae per year in the Milky Way and about 20 in other galaxies
 * absolute magnitude <math>M_V = -8 mag</math>
-* spectra of novae near maximum light resemble A-F absorption spectra of luminous stars at first
+* spectra near maximum light resemble A-F absorption spectra of luminous stars at first
 * amplitude between 7 and 19 mag in V
 * quick rise of few days

← Older revision		Revision as of 13:46, 28 July 2009
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	* slow decline, between few days and 100 days (fast: type A, slow: type B, very slow: type C)		* slow decline, between few days and 100 days (fast: type A, slow: type B, very slow: type C)
	* 15 days after maximum its Mv = -5.5mag, independent on speed or class		* 15 days after maximum its Mv = -5.5mag, independent on speed or class
		+
		+	'''Recurrent novae''':
		+	* are produced by a white dwarf star and a red giant circling about each other in a close orbit
		+	* recurrent every 10-100 years
		+	* smaller amplitude: 4-9 mag
		+	* M_V at minimum is about 0-1 mag
		+	* example: RS Oph - 3 outbursts between 1957 and 1991 (AAVSO), exhibits some small variation in the baseline in minimum
		+	* decline within few days