The Impossible Star
astrobites.org
astrobites.org
"These dips could have been caused by a planet orbiting the
binary system, but in 2013, a different group proved that
the third object must be a star. They did this by finding
variations in the orbital period of the binary, variations
caused by the changing light travel time as the binary
orbits a third star."
Translated: the binary star system is co-orbiting a third object, whose pull on the binary is so strong that it must be star-sized rather than planet-sized. How do they measure this pull? It's a Doppler effect -- not the familiar one, a shift in the frequency of waves (like sound) -- but a shift in the frequency of the binary star orbit! This orbit is a clock with a constant 0.258 day period between ticks. When the binary is moving towards earth, these clock ticks are "catching up" [0] with the starlight moving towards earth -- they're compressed together, so the binary looks like it's orbiting faster than it actually is! If you measure this Doppler shift, how it changes as the binary orbits the third star (first moving slightly faster towards earth, then away from it), you can infer the speed of its orbit around the third star -- and from that, the mass of the third star!I was just reading about this recently: I was going to say (wrongly) this technique was used by in the 17th century to measure the speed of light, by measuring a Doppler shift of the orbital period of Jupiter's moon Io [1]. In fact Ole Rømer measured the phase of Io's orbit, rather than the frequency. You can track Io's orbit phase very exactly by timing the moment it falls behind Jupiter's horizon (a regular eclipse). With Io's orbit as a clock located at Jupiter (the eclipse moment as the "tick"), you can measure differences in light travel time from Jupiter to Earth as they move apart. This is a phase measurement, not frequency; and it depends on the Jupiter-Earth distance, not their relative speed.
[0] Like this GIF: https://en.wikipedia.org/wiki/Doppler_effect#mediaviewer/Fil...
[1] https://en.wikipedia.org/wiki/Rømer's_determination_of_the_s...
(§8.2 says my confusion is a common one, so there!)
(Also, don't confuse this with doppler spectroscopy [2] -- measuring shifts in the frequency (color) of light, rather than the frequency of orbits. This is the "Doppler" that's used to discover exoplanets!)
I found that a fascinating thought, so I looked up other binary stars and found there's one with a period of ~17 minutes. http://en.wikipedia.org/wiki/Orbital_period#Binary_stars
https://en.wikipedia.org/wiki/AM_Canum_Venaticorum
Both of the stars stars are white dwarves, a mass of a sun squeezed into the size of a small planet. With a 17-minute orbit, they're incredibly close: one of them is ripping the atmosphere off of the other. Helium from the lighter dwarf is being pulled off and falling onto the more massive one -- pulled so strongly, it impacts the surface at several percent the speed of light. A helium layer builds up, at temperatures and pressures close to that of the interior of a hydrogen bomb. And at some point it does go off, like a hydrogen bomb -- a thermonuclear detonation the size of a planet, the entire surface igniting almost simultaneously. And this keeps repeating!
The area of Earth is around 5 × 10^8 km^2. So, 'planet size', that's about 10^11 tons TNT per square km, or 2,000 Tsar Bomba's per square km (Tsar Bobma was around 5-6 × 10^7 ton TNT equivalent).
Volume-wise, it would be about one Tsar Bomba per cubic kilometer of Earth.
So yes, I guess you could call that planet sized.
The TNT equivalent of the 50 Mt test could be represented by a cube of TNT 312 metres (1023 feet) on a side, approximately the height of the Eiffel Tower.
Which when you carry with your numbers, means that more than 9 (3^3) but much less than than 64 (4^3), (excuse the massive lack of accuracy but I'm doing a fermi estimate here, it seems appropriate) which are both massively less than 2000, which means that, the explosion you would get if you covered the earth with a 10Km 'crust' of TNT, would still not be bigger than this star when it goes off.Id definitely call that planet sized.
> These quadruple models yield reasonably good fits to the data, and are physically possible, which is an improvement over the triple model!
Brilliant. Just noticed the author of the paper is from my alma mater, too.
However, imagine being a species on such a planet, and trying to work out astronomy. Motions of objects in the sky would be rather confusing. To put it mildly.