Sky & Telescope - June 2024 - 17

masses in these extragalactic events were larger than galactic
sources like V1309 Sco. It emerged that the more massive
the stellar pair, the brighter a flash they produced as they
fell together. In fact, a merger of a 10-solar-mass star with a
companion is about 1,000 times brighter than a similar event
involving a 1-solar-mass star.
Recently, other similarities have come to light. Despite
their range of masses, all of the stars' pre-outburst rises in
brightness shared similar colors. The members were also relatively
compact stars that had just stopped burning hydrogen
in their cores, partway along their evolution toward becoming
red giants. They tended to be blue or yellow stars, of spectral
types B through G.
Missing among all of these blue and yellow progenitor
stars, however, were the puffiest, reddest giants - stars like
what the Sun will evolve into in another several billion years.
These missing events are now turning up as " redder than red "
novae: outbursts that happen at such cool temperatures that
they only glow in infrared light.
Searches for these events began with NASA's Spitzer Space
Telescope and are continuing now using NEOWISE and the
James Webb Space Telescope. These discoveries have taught
us that collisions involving aging red stars look substantially
different than the other stellar crashes we've seen.
When a relatively hot star like the Sun merges with a
companion, we see a red nova that starts out bright in visible
light before eventually giving way to a dusty, infrared-bright
aftermath. When a cooler star (like an old, fluffy red giant)
swallows a companion, the whole process is slower and less
energetic. The traces are dusty and infrared-bright from the
start, with visible light enshrouded by the curtain of dust the
stars spew out as they coalesce.
D
15
16
17
18
19
20
−10 0 10 20 30 40 50 60
Time from outburst peak (days)
140
C
70
140
D
70
I
V
C
R
ANATOMY OF A RED NOVA As the stars spiral
in toward each other, they throw off gas, and the binary
brightens. Here, light curves at different visible
and infrared wavelengths for the red nova in M31
are paired with the author's simulation snapshots,
which show the lead-up to the stars' merger. The
simulation looks at the binary from above, showing
gas density in the orbital plane. Brighter areas show
where gas is denser. The white circle is the primary's
core; the white star is the secondary's core. (In the
inset light curve, BVRI are specific visible and nearinfrared
filters, from bluer to redder in color.)
B
−70
−70
−140
−140
−140
−70
Distance (solar radii)
70
140
−140
−70
Distance (solar radii)
sk yand tele scope .o r g * JUNE 2024 17
70
140
Distance (solar radii)
Apparent magnitude
Distance (solar radii)
http://skyandtelescope.org

Sky & Telescope - June 2024

Table of Contents for the Digital Edition of Sky & Telescope - June 2024

Contents
Sky & Telescope - June 2024 - Cover1
Sky & Telescope - June 2024 - Cover2
Sky & Telescope - June 2024 - 1
Sky & Telescope - June 2024 - Contents
Sky & Telescope - June 2024 - 3
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