From galaxy mergers we now turn to Black Hole mergers.
TMaximum Black Hole Mass Across Cosmic Time
Jorick Vink
This is a weird system with 2 larger then necassarily steller mass systems merging into an intermediate mass Black Hole!
Q - What is max mass of Star/BH?
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It was thought that as steller masses increase, steller winds increasm causing more and more material to be lost through wind, and lower the max mass of the star. BUT… is this always true?
No - stars with lots of metals have more possible spectral lines and lower max mass
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On the other hand, if you have very very low metallicity stars - stars missing heavy atoms - then stars can get much much bigger, and bigger black holes can result from the evolution of a single star.
Stars even up to 100 solar masses!
This can lead to the 85 solar mass BH
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This work is getting published in Vink et al 2021, MNRAS 504,146.
Final result: The maximum black hole mass changes over time, with larger mass black holes forming from earliest stars.
Personal comment: This does not mean all 85 solar mass BH’s come from single stars.
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It is still not easy to go from potential formation of 85 solar mass Black Holes to the formation of supermassive black holes via mergers. Another story likely still needed to explain the earliest massive black holes in the cores of galaxies, but that’s ok. More science!
/fini
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The 2nd presentation in today’s first #AAS238 presser looks at ways to find planets by looking at the composition of stars.
A Statistical Search for Chemical Signatures of Planet Formation in Sun-like Stars
Jacob Nibauer (University of Pennsylvania)
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There was a lot of chemistry in this talk, but the bottom line is this: If you have two stars that formed from the same kind of stuff, then the star that forms rocky worlds will have less of the stuff needed to make those planets then a star that didn’t make planets.
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To test this concept, need to cross-match Kepler & TESS exoplanet hosts to identify if they do or don’t show expected depletions, need to consider binaries.
I’m curious if we have enough data to consistently say, here are rocky worlds, & here aren’t rocky worlds?
First presentation looks at CHIME and Fast Radio Bursts!
Fast Radio Bursts: From a Handful to Hundreds with CHIME/FRB
Kiyoshi Masui (MIT), Alex Josephy (McGill University) & Mohit Bhardwaj (McGill Univ.)
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CHIME is a cool Canadian radio array nicely tuned to the colors of radio light where whatever is causing Fast Radio Bursts (FRBs) are doing their primary bursting.
We really don’t know a lot about FRBs. They are (astronomically) pretty new discoveries, every obs is needed.
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FRBs are brief, & to see them you need to either be looking exactly right by luck, or looking everywhere by design.
CHIME uses sophisticated data processing to look at most of visible sky simultaneously, and tune in fast.
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In just a couple years, known catalogue grew a lot!
Ok, seminar stuff about this giant new shiny IR telescope that may or may not launch later this year.
So far, it’s the same info seen since I was in grad school, but with better images & animations.
Reminder, JWST was supposed to launch in 2007.
No, I’m not bitter.
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This presentation is acknowledging how ALMA is really doing amazing science that we really thought would have to wait until JWST launched.
Scientists will find a way to science!
This ground-based array is using its limited wavelengths to see star+Planet formation.
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From the ground, our atmosphere blocks & blurs many molecular lines - like water - but if JWST works (how do you say “break a leg" in telescope?) it will see more details, & will see what science data is blocked by our atmosphere’s water.
The Molecular Content of Planetary Nebulae: The Next Level
Kate Gold & Deborah Schmidt
and we are starting with super pretty images. I *need* to find this mosaic of Planetary Nebulae.
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We know basics of Planetary Neb (PN). Middle mass stars stop fusing materials in their core, exhale their atmospheres into nebulae, & that material gets recycled into future gen of stars. Since the PN are made of material enriched in the star, they have lots of MOLECULES.
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In this study, Gold & Schmidt observed a series of PN with different ages to see what is in them over time. They looked specifically for HCN & HCO+ in 30 PN and found they are common & seem to date back to star. This means molecules form in star & survive nebula formation.
Eta Carinae's Change of State as Seen by Hubble from 1998 to 2021
Kris Davidson, University of Minnesota
Eta Car failed to go SN in the past but will likely go boom in the future. AND it’s only 7500ly away.
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Davidson reminds us at #AAS238 presser that Eta Car was one of the brightest stars in the sky… until it wasn’t. In 1800s there was a great eruption but then the star fadded away… only to slowly rebrighten again. It continues to work its way back to bright.
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Eta Car is actually 2 stars: a giant & a companion. They orbit every 5.5 yr & have a highly elliptical orbit that causes them to get much closer every 5.5 years. In the past, during this close passing, massive star dumped so much matter on companion it blocked UV.
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