Fair enough, I got the mechanism wrong, but aren't larger stars than our own more common? I thought in order to have stars like red and yellow giants with proportionally larger planets like the super-Jovians and super-Earths, it would require the system to form from the remnants (super/hypernovae clouds) of larger first-generation stars, the heavier ones that would have had the ability to fuse elements to the Uranium part of the table?
No, larger stars are less common. As a rule, the smaller a type of object is, the more common it is. Pretty intuitive, really, since you can make a bunch of small things out of the same amount of stuff as one big thing. The vast majority of stars in the galaxy are small red dwarfs, while big stars are much more rare, and also much shorter-lived. Remember, the paper that inspired this thread is about superterrestrial planets around red dwarfs, which is a big deal because red dwarfs are by far the most abundant type of star. So if Earthlike planets are common around them, there could be far more Earthlike planets in the galaxy than we used to think.
And stars don't fuse elements heavier than iron, except during supernovae. Fusing elements lighter than iron is exothermic: you get more energy out of it than you put into it. So that kind of fusion can produce energy and be self-sustaining as a stellar fuel source. But fusing elements heavier than iron is endothermic -- you get less out than you put in. So once fusion in a giant star's core turns it into iron, the fusion stops dead and all the mass of the star collapses in on itself with such force that the star blows up. And that titanic explosion generates enough energy to fuse elements heavier than iron -- as well as distributing all the other elements that were created in the core but mostly trapped within the star during its lifetime.
So the first-generation stars wouldn't have had any elements heavier than iron in them, not until they blew up. Since heavy elements are only introduced into the galaxy by supernovae, the percentage of heavy elements in the universe has increased over time. The oldest star systems are much more metal-poor (and to astrophysicists, "metal" means "anything heavier than helium"). This is one of the ways we determine the age of a star system, by measuring the metallicity in its spectrum. Younger stars and planets form out of material that's been more enriched by heavy elements spewed into space by supernovae.
This is part of why it's surprising to find so many superterrestrials around red dwarfs. They're the longest-lived category of star, so statistically speaking, a lot of them would be very old and metal-poor. We didn't expect to find big planets around them. And we can't yet make any assumptions about how rich those planets are in heavier elements. Many of them might be big but light, made mostly of rock and ice with little metal, which would give them relatively lower gravity.