Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Aquila |
Right ascension | 19h 23m 05.30s [1] |
Declination | 04° 57′ 19.1″ [1] |
Apparent magnitude (V) | 3.9 Max. 17.1 Min. [2] [3] |
Characteristics | |
Variable type |
Classical Nova
[3], eclipsing binary [4] |
Astrometry | |
Parallax (π) | 0.5615 ± 0.1281 mas [5] |
Distance | 1,239+422 −127 [3] pc |
Absolute magnitude (MV) | −8.2 Max. 4.8 Min. [2] [3] |
Orbit [6] | |
Period (P) | 0.1346 days |
Semi-major axis (a) | 1.17 - 1.24 R☉ |
Inclination (i) | 78.5 [7]° |
Details | |
white dwarf | |
Mass | 0.92 - 1.13 [6] M☉ |
Luminosity | 750 - 3,000 [7] L☉ |
Temperature | >100,000 (2000) [8] K |
donor | |
Mass | 0.28 [6] M☉ |
Temperature | 3,000 [7] K |
Other designations | |
Nova Aquilae 1999 b,
AAVSO 1918+04 | |
Database references | |
SIMBAD | data |
V1494 Aquilae or Nova Aquilae 1999 b was a nova which occurred during 1999 in the constellation Aquila and reached a brightness of magnitude 3.9 on 2 December 1999. [2] making it easily visible to the naked eye. [9] The nova was discovered with 14×100 binoculars by Alfredo Pereira of Cabo da Roca, Portugal at 18:50 UT on 1 December 1999, when it had a visual magnitude of 6.0. [10]
V1494 Aquilae is classified as a fast nova, meaning it faded from peak brightness by more than 3 magnitudes in less than 100 days. [11] During its decline, V1494 Aql produced unusual variations in its x-ray radiation, including a bright burst lasting several minutes. During 2000, the x-ray spectrum developed from a hard (high energy) emission-line spectrum to a spectrum typical of a super soft X-ray source. The x-ray intensity varied with a period of about 40 minutes, probably due to pulsations induced in the white dwarf by its re-kindled hydrogen fusion. [8]
All novae are binary systems with two stars orbiting so close to each other that one star, the "donor" star transfers matter to the other star which is a white dwarf. In the case of V1494 the white dwarf has a mass of 1.20 M☉, and it is accreting mass from the donor star at a rate of 2.1 × 10−10 M☉ yr−1. [12] The stars' orbital period is 3.23 hours, [11] and the system is an eclipsing binary with two brightness minima each orbit, one 0.5 and one 0.1 magnitudes deep. [2] [4] This apparently is a measurement of two stars of approximately equal brightness, the nova and a companion 1.4 ″ to the south east. Measuring only the brightness of the nova, the eclipses are about two magnitudes deep. [13] The white dwarf is probably an oxygen-neon-magnesium type. [6]
Unlike some novae, the material ejected from V1494 Aquilae has not formed a visible nebula around the star. [14] However, a shell approximately 6.5 ″ across has been detected spectroscopically in H-alpha emission. [13]
The distance to V1494 Aquilae has been estimated by different methods. Early estimates were based on assumptions about the luminosity of the nova and gave distances around 1.2
kpc.
[7] Later models assumed distances of up to 2.2 kpc.
[6] Comparison of the measured shell size with the observed expansion velocity give a distance of 1.2±0.2 kpc.
[13]
Gaia DR2 published a parallax of 0.8394±0.1415
mas, corresponding to a distance of 1,239+422
−127 kpc.
[3]
Gaia EDR3 published a parallax of 0.5615±0.1281 mas, corresponding to a distance around 1,800 kpc.
[5]
Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Aquila |
Right ascension | 19h 23m 05.30s [1] |
Declination | 04° 57′ 19.1″ [1] |
Apparent magnitude (V) | 3.9 Max. 17.1 Min. [2] [3] |
Characteristics | |
Variable type |
Classical Nova
[3], eclipsing binary [4] |
Astrometry | |
Parallax (π) | 0.5615 ± 0.1281 mas [5] |
Distance | 1,239+422 −127 [3] pc |
Absolute magnitude (MV) | −8.2 Max. 4.8 Min. [2] [3] |
Orbit [6] | |
Period (P) | 0.1346 days |
Semi-major axis (a) | 1.17 - 1.24 R☉ |
Inclination (i) | 78.5 [7]° |
Details | |
white dwarf | |
Mass | 0.92 - 1.13 [6] M☉ |
Luminosity | 750 - 3,000 [7] L☉ |
Temperature | >100,000 (2000) [8] K |
donor | |
Mass | 0.28 [6] M☉ |
Temperature | 3,000 [7] K |
Other designations | |
Nova Aquilae 1999 b,
AAVSO 1918+04 | |
Database references | |
SIMBAD | data |
V1494 Aquilae or Nova Aquilae 1999 b was a nova which occurred during 1999 in the constellation Aquila and reached a brightness of magnitude 3.9 on 2 December 1999. [2] making it easily visible to the naked eye. [9] The nova was discovered with 14×100 binoculars by Alfredo Pereira of Cabo da Roca, Portugal at 18:50 UT on 1 December 1999, when it had a visual magnitude of 6.0. [10]
V1494 Aquilae is classified as a fast nova, meaning it faded from peak brightness by more than 3 magnitudes in less than 100 days. [11] During its decline, V1494 Aql produced unusual variations in its x-ray radiation, including a bright burst lasting several minutes. During 2000, the x-ray spectrum developed from a hard (high energy) emission-line spectrum to a spectrum typical of a super soft X-ray source. The x-ray intensity varied with a period of about 40 minutes, probably due to pulsations induced in the white dwarf by its re-kindled hydrogen fusion. [8]
All novae are binary systems with two stars orbiting so close to each other that one star, the "donor" star transfers matter to the other star which is a white dwarf. In the case of V1494 the white dwarf has a mass of 1.20 M☉, and it is accreting mass from the donor star at a rate of 2.1 × 10−10 M☉ yr−1. [12] The stars' orbital period is 3.23 hours, [11] and the system is an eclipsing binary with two brightness minima each orbit, one 0.5 and one 0.1 magnitudes deep. [2] [4] This apparently is a measurement of two stars of approximately equal brightness, the nova and a companion 1.4 ″ to the south east. Measuring only the brightness of the nova, the eclipses are about two magnitudes deep. [13] The white dwarf is probably an oxygen-neon-magnesium type. [6]
Unlike some novae, the material ejected from V1494 Aquilae has not formed a visible nebula around the star. [14] However, a shell approximately 6.5 ″ across has been detected spectroscopically in H-alpha emission. [13]
The distance to V1494 Aquilae has been estimated by different methods. Early estimates were based on assumptions about the luminosity of the nova and gave distances around 1.2
kpc.
[7] Later models assumed distances of up to 2.2 kpc.
[6] Comparison of the measured shell size with the observed expansion velocity give a distance of 1.2±0.2 kpc.
[13]
Gaia DR2 published a parallax of 0.8394±0.1415
mas, corresponding to a distance of 1,239+422
−127 kpc.
[3]
Gaia EDR3 published a parallax of 0.5615±0.1281 mas, corresponding to a distance around 1,800 kpc.
[5]