From: Dagon Gmail (dagonweb@gmail.com)
Date: Fri Dec 12 2008 - 07:01:37 MST
Hi
I have mailed this question to some specialists in the field but I can
understand they didn't have/take
the opportunity to answer me, but maybe SL4 have people aboard who consider
this a worthwhile
topic.
In short, I read that there have been pulsars detected with telltale
planetary wobble. This appears to be
easy, because neutron stars are small, very bright and have very precise
spectral signatures. Now
I am wondering about a few things . If you like to enlighten me, can anyone
please add "cinematic
desciptions"? *Just pretend you are instruction a movie director on how it
would look and he has to
make a realistic depiction of your descriptions.*
1 - how much hard radiation do these planetary companions experience. How
does that amount
compare to what the sun emits on average and during peak events (such as
when a comet slams into
a neutron star surface? What does energy of that magnitude do to stuff we
know? Say, a block of
iron a meter big at 1AE? To what can I compare these phenomena?
2 - neutron stars (pulsars) are very small objects, yet their surface
temperature (!!) reaches over a
billion degrees. Nevertheless these planets revolve about the stellar husk
at distances of at least millions
to hundreds of millions of klicks. At that distance even a pulsar would be a
point object. So how much
output does it have, compared to the sun? What is the composition of the
light compared to the sun?
3- I saw analysis that pulsars create light pressure of such vicious power
they can strip the gas of a
companion star that was under several million clicks away. How would such a
spiraling outawrd plume
of gas look when watched from a safe distance?
4 - Most loaded question that many people will resist answering - in purely
cinematic terms, how would
a pulsar look seen from "safe distance". What is safe distance? How would
pulsar planets look? How
strong are aurorae on such a planet compared with terrestrial aurora, and
how would they look? What
geochemistry processes would occur on a pulsar planet? Wouldn't a pulsar
strip any gaseous envelopes
away real fast?
5- when would a pulsar planet have formed - from pre-nova conditions, or
from coalesced (!!) post nova
material? Would a pulsar former after the main star when berzerk have a high
composition of materials
heavier than iron? Would a high element compostion of such a planetary body
cause it to heat up
relative to earth due to radioactive composition?
6 - what escape velocities relative to C would a neutron star, pulsar (quark
star, magnetar) have? What
would be the features of a heavy stellar remnant as it goes up in escape
velocity closer to C? What
auroric phenomena would a pulsar show, when viewed from a safe distance?
Would some of these objects
be anything else other than very bright? Would interstellar gas caught in a
pulsars beams light up?
Would the nova cloud of a pulsar be visible from within the system or is it
too dim? Would the light of
"very heavy" neutron stars "dim" due to "gravity well redshift"?
7- Do pulsars/neutron stars have a physiology other than that caused by the
sequence of the star,
spin and mass? Or there other formative elements that determine distinct
fysiological qualities (that have
distinct effect on their outward features) ? ... such as having been part of
a double system, with companion
material raining down on the star in an earlier epoch?
8- Neutron stars form when very big stars go supernova. I am stunned at the
idea that the very moment a
star stars fissioning out iron, the iron literally "absorbs" energy and the
star collapses in a minisecond.
Implicitly this means that these stars detonate with a more or less solid
iron core. That means they eject
a particularly large amount of heavy stuff. Would an area "close to" a
neutron star be seeded with stable
heavy elements? How would a nearby star (that was not in the blast range of
a GRB) experience a
supernova? Would it notice supernova ejecta "raining in" after a decade?
Thanks, anyone.
This archive was generated by hypermail 2.1.5 : Wed Jul 17 2013 - 04:01:03 MDT