Spectroscopic Study Of Light Curve And Physical Properties For SN2010jl

In this work, The physical properties were studies for (supernova 2010jl)-which discovered on 2010 Nov. 3-depending on (Oort Model), optical spectrum curve and by applying special mathematical equations. The physical properties represented by explosion energy, initial velocity of ejecta, mass of ejecta, mass of 56Ni, distance from the earth, radius of ejecta, the momentum, expansion velocity and the age. Also, temperature of black body of SN2010jl during photospheric phase were calculated depending on data taken from optical spectrum curve and by applying special mathematical equation. The curve between temperature of black body and time in days were plotted, rang of temperature between (7300°k–9700°k) noticed .


Introduction
Supernova represents the catastrophic explosion that marks the end of the life of stars that have enough mass to explode,it is extremely luminous, and cause a burst of radiation that often briefly outshines an entire galaxy before fading from view over several weeks or months [1]. During this short time a supernova can radiate as much energy as the Sun is expected to emit over its entire life. During the explosion much or all of a star's material will be ejected at a speed of about (0.1c), driving a shock wave into the surrounding interstellar medium that sweeps up an expanding shell of gas and dust called a "supernova remnant" which continues to expand over millions of years until it dissolves into the interstellar medium.
Supernovae are very rare events occurring once or twice per centuries in a galaxy. Historical records, particularly the careful data recorded by the Chinese, show that seven or eight supernovae have exploded over the last 2000 years in our galaxy. But even though they are very rare events, they play a * Corresponding author at: AL-Mustansiriyah University -College of science; ORCID: https://orcid.org/0000-0001-5859-6212 .Mobil:777777 E-mail address: significant role in enriching the interstellar medium with heavy elements (up to iron) and they are the source of most radio waves, X-rays, and cosmic rays in the universe. In addition to that, it releases a huge amount of energy that heats up the interstellar medium and triggers the formation of stars in the galaxy [2].
As the observation techniques and astronomical instruments improved more and more, supernovae have been discovered each year, reaching by now to more than thousands of supernovae. Supernovae do not have complicated creative names; they are named after the year in which they are discovered and in the order they are discovered, consequently the first supernova discovered in the year will take the first uppercase letter in the alphabet (A) placed after the year of discovery, for example SN 1987A represent the first supernova discovered in 1987, the second supernova discovered in the same year will take the letter B and so on for other supernovae. But if more than 26 supernovae are discovered in the same year (as has been the case since the mid-eighties) the 27th is given the suffix "aa", the 28th is thus "ab" and so on. Once all the "a" have been exhausted, "b" are used, i.e. "ba", "bb", and so on, for example the last supernova discovered in 2010 was known as SN 2010lt which means that this supernova is number 332th supernova that was discovered in 2010 [3]. Mʘ yr -1 [5,6]. for typical Type IIn supernovae (SNe IIn) [7] The mass loss can be up to several Mʘ extending out as far as 10 17 cm.
The class of ultraluminous supernovae overlaps the SNe IIn, with objects like SN 2006gy that was very bright for 240 days and radiated ≥2 × 10 51 ergs in optical light [8]. Another group of the ultraluminous events are not SN IIn, but have spectra that resemble SNe Ic at later times [9,10]. Chevalier & Irwin [8] suggested that the ultraluminous supernovae are due to dense circumstellar interaction, but only ones with a circumstellar extent greater than the radius at which radiation can diffuse out have Type IIn characteristics.
The mass loss involved can be ≥ 10Mʘ and extends to ≥ 2 × 1015 cm for Type IIn characteristics. To account for such high mass loss rates, luminous blue variable (LBV) progenitors have been suggested [11].
The implication is that SN IIn progenitors are not confined to very high mass stars, but may cover a broad range of stellar masses. These properties argue against a particular mass range becoming a supernova, and indicate that some factor other than mass plays a role. Here we suggest that the factor is binarity and that the mass loss and explosion are both driven by the inspiral of a compact object in common envelope (CE) evolution [12] .

SN2010jl
On 2010 Nov 3.5 a supernova was discovered in the galaxy UGC 5189A, located about 160 million light years away. Using data from the All Sky  [13].

THEORETICAL PART
From the spectrum of SN2010jl in the earlier stage, shown in (Fig 1 ), the initial radial velocity of the ejecta (υ) can be found by using the the emission

1-Oort Model:
Oort model is a model that was performed by Substituting equation (8) in equation (7) and integrate, we get: On the other hand the radius of the remnant is relatively small and has a current value about 0.186 pc, and this is also due to the large density of the surrounding circumstellar medium that prevents the shock wave from expanding further.

2-Results of Temperature of Black Body
According to Fig. (2) [24],and by get data program we get tables (3) and (4), after that we plot between values of (B-V) and time in days Fig.(4), also between temperate of black body for SN2010jl with time in days Fig.(5). The supernova starts out very hot and cools off, as would be expected. The cooling leves off at approximately 6000°k . At this point, the ionized hydrogen shell has started recombining and deeper shells in the envelope become visible. This graph only shows the temperature for the first one hundred days: the photospheric phase. Once the supernova enters the nebular phase, a blackbody is no longer a good approximation.
From Fig (4), the color curves kept nearly a constant for SN 2010jl during the phase from t ≈ 29 days to t ≈ 176 days after the maximum. That the shape of the continuum spectra did not change significantly during this period, which is consistent with that the blackbody temperature from the spectra stays at range ≈( 7000°K -9000 °K) at similar phases.

CONCLUSION
The remnant is still in the free expansion phase since the sweeping mass is still smaller than the ejected mass. The remnant has expanded into a radius equal 0.186 pc during the past 2 years with current velocity 2920 km.s -1 . The BVRI light curve of SN2010jl appears to be generally similar to other "typical" type IIn supernova .