RS Ophiuchi
Sanarahamat A Kodake
Hrithik
Physics@IIT Delhi
RS OPHIUCHI
• recurrent nova system
• 5,000 light-years away
•
constellation Ophiuchus
• apparent magnitude of about 12.5.
• 1898, 1933, 1958, 1967, 1985,
2006 and 2021
RS OPHIUCHI
• Red giant secondary (M2 III)
•
Massive White dwarf ∼ 1.35 M⊙
• Frequent eruptions- High mass of WD and high accretion rate
• Mass may reach chandrashekhar limit
• Explode as type 1a Supernova
• Early stage- broad low ionization lines
• Nebular stage with strong coronal line
[Fe XIV] 0.5303 µm,
[Ar X] 0.5535 µm,
[Fe X] 0.6374 µm,
[Si VI] 1.9641 µm,
[Al IX] 2.0444 µm, [Mn XIV] 2.0894 µm)
• Shock wave discovery
DATA COLLECTION
Day-31
Optical March 15
NIR
March 16
Day-49
Optical April 4
NIR
April 2
Observatorio Astronomico
Nacional en San Pedro
M´artir/ Boller & Chivens
32 Mt. Abu Telescope/NICMOS
Astrophysical Observatory of
Asiago/ Boller & Chivens
Mt. Abu Telescope/ NICMOS
MODEL PARAMETERS
1.
Temperature of central source and shape
2.
Luminosity
3.
Inner and Outer radii
4.
Hydrogen density at illuminating part
5.
Covering factor
6.
Fill factor
7.
Abundances of different elements
8.
Exponents for hydrogen density and fill factor
INPUT SCRIPT
INPUT SCRIPT
OUTPUT :COMPARISON
OF OBSERVED AND
MODELLED SPECTRA
1. Visible Band
2. J-band
3. H-band
4. K-band
ESTIMATION OF THE
EJECTA MASS
We can estimate the hydrogen ejected mass predicted by the two
component models using the following relation.
Ejected mass for D31 is found to be 3.4 × 10-6 M⊙
CONCLUSION
• generated a set of spectra by varying several parameters and
assuming a spherical geometry of the ejecta that consists of
two different shells of different densities.
• The best-fit model parameters are in agreement with a hot WD
with temperature of 5.5-5.8*105 K and luminosity of 6-8*1036
Erg s -1
• The abundance analysis shows that the ejecta are significantly
enhanced, relative to solar, in helium, nitrogen, neon, iron and
argon as well as silicon was found to be subsolar.
THANK YOU