Astronomy C

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bhavjain
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Astronomy C

Postby bhavjain » September 6th, 2016, 9:00 pm

Short Event Description: Teams will demonstrate an understanding of stellar evolution and Type Ia supernova.

What is a Type 1a supernova, and how does it differ from a Type II supernova?
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Re: Astronomy C

Postby slowpoke » September 6th, 2016, 9:15 pm

idk astro tbh
a supernova that occurs in a binary system with one of the bodies being a white dwarf (and the white dwarf is the one going supernova); it is different from a type ii supernova because it contains no hydrogen lines in its spectrum and contains one of silicon
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Re: Astronomy C

Postby bhavjain » September 6th, 2016, 9:26 pm

Correct! Also, a type II supernova results from the collapse of a massive star's iron core. Your turn.
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Re: Astronomy C

Postby slowpoke » September 8th, 2016, 11:37 pm

Explain how a type 1a supernova occurs from a double degenerate progenitor.
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Re: Astronomy C

Postby bhavjain » September 9th, 2016, 7:24 am

slowpoke
Answer
Two white dwarfs merge and their combined mass exceeds the Chandrasekhar limit (1.39 solar masses), forming a type 1a supernova.
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Re: Astronomy C

Postby Magikarpmaster629 » September 9th, 2016, 8:05 pm

slowpoke
Answer
Two white dwarfs merge and their combined mass exceeds the Chandrasekhar limit (1.39 solar masses), forming a type 1a supernova.
Just want to point out that the Chandrasekhar limit is usually written as ~1.4, since it has variations too great for a significance of 0.01 (although I remember seeing 1.44, not 1.39). This is further complicated by the fact that in some cases white dwarfs can surpass the Chandrasekhar limit without exploding.
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Re: Astronomy C

Postby bhavjain » September 9th, 2016, 8:08 pm

Magikarpmaster629 I see it as 1.4 as well, but https://en.m.wikipedia.org/wiki/Chandrasekhar_limit says 1.39. What do you mean by significance of .01?
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Re: Astronomy C

Postby slowpoke » September 9th, 2016, 8:27 pm

slowpoke
Answer
Two white dwarfs merge and their combined mass exceeds the Chandrasekhar limit (1.39 solar masses), forming a type 1a supernova.
That is essentially correct! Your turn.
Magikarpmaster629 I see it as 1.4 as well, but https://en.m.wikipedia.org/wiki/Chandrasekhar_limit says 1.39. What do you mean by significance of .01?
I personally use 1.44 after a lot of scourging around online. However, I recently read an article saying that the limit decreases with increasing central density and gravity considerations from ~1.46 so it may be safer to put 1.4 or something else. However, I would say as a general guideline to not trust wikipedia definitively on every number it gives you and to do your own research outside of that.
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Re: Astronomy C

Postby Magikarpmaster629 » September 12th, 2016, 3:03 pm

This QM is severely laking in math...

The system 'Beta Constellationi' contains two stars, A and B. It has a measured trigonomic parallax of 0.03 arcseconds and the angular size of the semi-major axis is 2.93 arcseconds. The system takes 465.5 years to fully orbit.

1. What is the distance to the system in parsecs?
2. What is the actual distance between stars A and B in AU?
3. What is the mass of the system? Give your answer in solar masses.
4. The distance from the center of mass of the system (also known as the barycenter) to star A is 60 AU. What is the distance to star B from the barycenter?
5. What are the individual masses of stars A and B?
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Re: Astronomy C

Postby Unome » September 12th, 2016, 3:45 pm

This QM is severely laking in math...

The system 'Beta Constellationi' contains two stars, A and B. It has a measured trigonomic parallax of 0.03 arcseconds and the angular size of the semi-major axis is 2.93 arcseconds. The system takes 465.5 years to fully orbit.

1. What is the distance to the system in parsecs?
2. What is the actual distance between stars A and B in AU?
3. What is the mass of the system? Give your answer in solar masses.
4. The distance from the center of mass of the system (also known as the barycenter) to star A is 60 AU. What is the distance to star B from the barycenter?
5. What are the individual masses of stars A and B?
Maybe I'll get more than one right
1. 33.33 parsecs 2. 97.66 AU? 3. uhhh... 1148120.12 solar masses? lol 4. 37.66 AU??? 5. if 3 and 4 are correct, A = 507518.948 solar masses and A = 640601.172 solar masses (iirc stars don't actually get this big, right?)
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Re: Astronomy C

Postby Magikarpmaster629 » September 12th, 2016, 4:03 pm

This QM is severely laking in math...

The system 'Beta Constellationi' contains two stars, A and B. It has a measured trigonomic parallax of 0.03 arcseconds and the angular size of the semi-major axis is 2.93 arcseconds. The system takes 465.5 years to fully orbit.

1. What is the distance to the system in parsecs?
2. What is the actual distance between stars A and B in AU?
3. What is the mass of the system? Give your answer in solar masses.
4. The distance from the center of mass of the system (also known as the barycenter) to star A is 60 AU. What is the distance to star B from the barycenter?
5. What are the individual masses of stars A and B?
Maybe I'll get more than one right
1. 33.33 parsecs 2. 97.66 AU? 3. uhhh... 1148120.12 solar masses? lol 4. 37.66 AU??? 5. if 3 and 4 are correct, A = 507518.948 solar masses and A = 640601.172 solar masses (iirc stars don't actually get this big, right?)
Stars don't get that big; you messed up on 3 and 5. 1, 2, and 4 are fine. You or someone else can try again.

EDIT: Actually there's a chance I messed up...the distance between the stars should be the same as the semi-major axis, but I could be wrong. Looking it up now.

EDIT 2: That does work...check Kepler's Third Law again.
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Re: Astronomy C

Postby Adi1008 » September 12th, 2016, 8:03 pm

Answer
1. 33.33pc 2. 97.66 AU 3. 4.298 solar masses 4. I'm not 100% sure what you mean - is this just supposed to be 97.66-60 = 37.66 AU? 5. B is 2.641085 solar masses, A is 1.6575 solar masses (these may be a bit off due to rounding along the way)
Unome, I think you might have forgot to cube or square something (but more likely the latter, since your answer is so large) while doing stuff with Kepler's Third Law. The most massive star, R136a1, is 265-375 solar masses, while a lot of theoretical estimates give a maximum mass of usually 70-300 solar masses.
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Re: Astronomy C

Postby Magikarpmaster629 » September 13th, 2016, 12:47 pm

Answer
1. 33.33pc 2. 97.66 AU 3. 4.298 solar masses 4. I'm not 100% sure what you mean - is this just supposed to be 97.66-60 = 37.66 AU? 5. B is 2.641085 solar masses, A is 1.6575 solar masses (these may be a bit off due to rounding along the way)
Unome, I think you might have forgot to cube or square something (but more likely the latter, since your answer is so large) while doing stuff with Kepler's Third Law. The most massive star, R136a1, is 265-375 solar masses, while a lot of theoretical estimates give a maximum mass of usually 70-300 solar masses.
Yeah, that's right.
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Re: Astronomy C

Postby Adi1008 » September 16th, 2016, 3:11 pm

(sorry for the late post!)

Consider the graph below, which shows two quantities for a white dwarf, mass and density, plotted as a function of radius. X-values increase going to the right, and y-values increase going up.

Image

(a) Which colored line shows the mass?
(b) Which colored line shows the density?
(c) What does this graph suggest about the relationship between mass and radius for this type of star?
(d) Is your answer to (c) also true for main-sequence stars?
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Re: Astronomy C

Postby Magikarpmaster629 » September 17th, 2016, 5:33 am

(sorry for the late post!)

Consider the graph below, which shows two quantities for a white dwarf, mass and density, plotted as a function of radius. X-values increase going to the right, and y-values increase going up.

(a) Which colored line shows the mass?
(b) Which colored line shows the density?
(c) What does this graph suggest about the relationship between mass and radius for this type of star?
(d) Is your answer to (c) also true for main-sequence stars?
a) Black
b) Red
c) There is an inverse relationship between mass and radius
d) No; they have a direct relationship
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