SN 2026aaiv Type 1a Supernova in Galaxy NGC 7331

The above image is a compilation of data obtained at the JPO using the Seestar S30 in EQ mode. 30 minute stack of 1minute exposures with the infra-red filter. Credit: Kurt Thrust.

" The JPO Team was pleased to capture the recently discovered Type 1a Supernova in the Galaxy NGC 7331 which was shining at approximately apparent mag 13.5. In reality and at peak, the absolute magnitude of a Type 1a Supernova is mag -19.3. As a guide our Sun's absolute mag is 4.8 (the scale is logarithmic and - denotes brighter than zero mag. Absolute magnitude is a common standard based upon how bright an object is if  placed at a standard distance of 10 parsecs where one parsec =32.6 light years). 

Galaxy NGC 7331 is 44 million Light Years distant and can be found in the Constellation Pegasus. It is mind blowing when considering the distances involved and the amount of energy released by the supernova. The above image was captured two nights ago on the 8th of August 2026, when the Supernova was more luminous than the combined output from the millions of stars at the galaxy's core. All typical Type 1a Supernova have the same absolute luminosity and consequently Type 1a Supernova are used as 'standard candles' in judging the vast distances to other galaxies. A Type 1a Supernova is estimated to generate 10^42 joules of energy, which is equivalent to the amount of energy the Sun will output over 10 billion years. The radioactive decay of nickel-56 and cobalt-56 powers the emission in visible light totalling approximately 10^49 ergs.

As the Galaxy is 44 million light years away (416272140793522000000 km), the photons of light energy, which our Seestar sensor collects, allow us to see a Supernova, which occurred 44 million years ago, as a live event. However, from the perspective of the photon travelling at light speed in a vacuum the journey is virtually instantaneous". - Joel Cairo CEO of the Jodrell Plank Observatory.

Enlarged  view showing SN 2026aaiv shining below and to the left of the less luminous galactic core. Image Credit: Pip Stakkert.

" We tried to obtain a low resolution spectrum from the Supernova using the Seestar and 'add on' diffraction transmission gratings' manufactured by our engineer, Jolene McSquint- Fleming. Unfortunately, a combination of issues associated with object low apparent luminosity and the shortness of sensor exposure times rendered our attempts unsuccessful. Further experimentation is underway on Jolene's bench". - Kurt Thrust current Director of the Jodrell Plank Observatory.

Saturn - South Pole

NASA’s Hubble Space Telescope images of Saturn (left) and a south-pole projection (right) highlight a newly tracked ten-sided atmospheric wave — a geometric counterpart to the long-known northern hexagon. Credit: NASA/ESA/STScI/Sánchez-Lavega et al. (ESA/Hubble heic2612a, CC BY 4.0).

"We thought this was an interesting post from NASA" - Joel Cairo CEO of the Jodrell Plank Observatory.  

"Astronomers have discovered a massive 10-sided atmospheric wave (a decagon) encircling Saturn’s south pole. Published in Science Advances in September 2026, the discovery was led by Agustín Sánchez-Lavega and compiled using observations from the NASA/ESA Hubble Space Telescope, ESO's Very Large Telescope, and ground-based amateur astronomers. 

 

​The structure provides a dynamic counterpart to Saturn's famous northern hexagon, which has been observed since the 1980s Voyager encounters.  

​Key Features of the Decagon

​Structure & Size: The decagon is a stationary-like wave pattern embedded within a high-speed eastward jet stream at southern mid-latitudes (around 58°S to 63°S). Each side measures roughly 10,000 miles (16,700 kilometers) across.  

​Wind Dynamics: While the encircling jet stream travels at speeds near 240 mph (400 km/h), the decagonal wave pattern itself drifts very slowly eastward at just 6 mph (10 km/h) relative to Saturn's rotation.  

​Vertical Depth: Observations in multi-wavelength infrared and visible spectrums demonstrate that the pattern penetrates down through multiple atmospheric cloud layers and haze, confirming it is a deep, 3D atmospheric wave rather than a shallow cloud-top feature".  Gary Gemini Coms Manager at the JPO.

​

Have Kurt and our Sponsor George Roberts gone 'Loopy' ? (Rhetorical)

 

The Cygnus Loop. Seestar S30 hybrid mosaic. Seestar in EQ mode, LP filter and 3.5 hours of 1 minute exposures in mosaic mode. Image Credit Kurt Thrust and Pip Stakkert. 

"Last night and early this morning were ideal for astro-imaging at the Jodrell Plank Observatory. 

As the weather forecasts for Lowestoft were predicting an extended period of cloud free skies over Suffolk, Kurt and George after some discussion, decided to use the Seestar S30 in EQ mode to image the entirety of the Cygnus Loop, using the little smartscope's firmware to create a mosaic of images as part of the capture process. 

The Moon didn't rise until quite early in the morning, so light pollution, which had plagued earlier attempts to image the Loop, was not a problem.

Unfortunately, minor mechanical or digital problems occurred, which meant the 'Eastern Veil' had to be added after the mosaic had been created and in post processing using the venerable but still excellent Registar software. 'Hats off ' to Olly Penrice who recommended purchasing this remarkable software to George many years ago.

Any how and irrespective of the processing route taken, the JPO Team were quite pleased with the end result"! - Joel Cairo CEO of the Jodrell Plank Observatory.

Enhanced Seestar Firmware stack showing flux and a multitude of stars within the plane of the Milky Way disc. Faint satellite trail removed using Google Gemini AI.

IC1396A The Elephant's Trunk Nebula.

 

The Elephant's Trunk Nebula in the Constellation Cepheus. Seestar S30 in EQ mode with Light Pollution Filter. 60x60 sec lights stacked and cropped post capture. Image Credit: Kurt Thrust.

" IC 1396A is one of the most photographed objects in the Northern Hemisphere sky. Strangely the JPO team had never imaged it before. So, with a one hour window of clear  sky over the Jodrell Plank Observatory, Kurt decided to point the Seestar S30 in its direction. The Seestar does well with large nebulae and for only one hour of exposures we thought this image, although 'crunchy', was not bad for a telescope having only 30mm of aperture.

We selected a colour palette in modified RGB, which follows the HOO narrow band palette in outline.

The above image captures IC 1396A, commonly known as the Elephant's Trunk Nebula, a dense globule of interstellar gas and dust embedded within the much larger ionized hydrogen region IC 1396, located in the high-northern constellation Cepheus approximately 2,400 light-years from Earth.

Astronomical Characteristics

• Morphology & Dynamics: The dark, elongated structure—resembling an elephant's trunk—is a dense molecular pillar sculpted by the intense ultraviolet radiation and high-velocity stellar winds emanating from the massive, luminous central O-type star HD 206267 (located just off-frame). The bright rim seen edging the dark structure is an ionization front, where radiation from HD 206267 heats and ionizes the outer compressed gas shell.

• Star Formation Site: The Elephant's Trunk is an active star-forming region (an H II region). The photoevaporative compression caused by nearby hot stars compresses the interior interstellar medium, triggering gravitational collapse and giving birth to young stellar objects (YSOs) and protostars hidden within the opaque dust lane.

• Spectral Emission: Captured using a light-pollution (LP) filter, the false-colour/dual-band palette Highlights the ionized atomic hydrogen (Halpha) emissions in warm amber and orange tones, while contrasting background dust lanes and surrounding ionized gas appear in cooler dark hues.

We will undoubtedly return to this object in the future, as more data will definitely improve image quality" - Kurt Thrust current Director of the Jodrell Plank Observatory.

The Elephant's Trunk Nebula an enlarged crop from the above wider field. Image Credit: Kurt Thrust.

Waning Gibbous Moon

 

Sometimes the Moon looks mysterious. Seestar S30 video clip stacked and processed post capture. Image Credit Pip Stakkert.

"Sometimes the Moon looks mysterious

Sometimes it appears cold and lonely

Sometimes it seems close

Sometimes far away

Sometimes it is a source of light pollution

But always, the Moon is Mozart's Queen of the Night"

Joel Cairo CEO the Jodrell Plank Observatory.

" The crater Aristarchus in top left, reflective and bright" - Kurt Thrust current Director of the Jodrell Plank Observatory.

This flyover was produced by the LPI's 2010 Lunar Exploration Summer Intern Program. The team members responsible for this work are Jean-François Blanchette-Guertin, Jessica Flahaut, Christie Jilly, Pryianka Sharma, and Audrey Souchon. Dr. David Kring acted as the interns' supervisor. Support for the program was provided by LPI and the NASA Lunar Science Institute (NLSI). USRA.

The Cygnus Loop an overview

 

The Cygnus Loop a collection of composite images captured with the JPO's Seestar S30 in August and September 2026. Image Credit: Kurt Thrust.

" We wanted to put together a panorama of individual images captured with the Seestar S30 to show the full extent of the Cygnus Loop in the constellation Cygnus the Swan. The Loop is quite large, 3 degrees in diameter, which is roughly equivalent to forty-five times the area presented by the Moon.  Unfortunately, the night Kurt chose to capture the data started well but as the night proceeded conditions deteriorated, as the Moon rose and the clouds appeared. Consequently, the above composite image uses the best data we have from two or more autumnal nights". - Joel Cairo CEO of the Jodrell Plank Observatory

"This image presents a composite astronomical collage showcasing key sub-regions of the Cygnus Loop (Sharpless 103), a large supernova remnant located approximately 2,400 light-years away in the constellation Cygnus. The mosaic brings together distinct narrow-band emission structures captured through astronomical imaging, highlighting the expanding shockwaves produced when a massive star exploded thousands of years ago.

Western Veil Nebula (NGC 6960 / The Witch's Broom)

Visible on the right side of the collage, the Western Veil exhibits delicate, filamentary shock fronts predominantly glowing in the light of ionized hydrogen (H alpha) and doubly-ionized oxygen (O III). The bright, central foreground star silhouetted along the filament is 52 Cygni, an unrelated spectroscopic binary that serves as a primary visual landmark for this segment of the remnant. The linear, swept-back tendrils illustrate where the expanding blast wave is encountering interstellar clouds, compressing and heating gas to tens of thousands of Kelvin.

Eastern Veil Nebula (NGC 6992 / NGC 6995)

Positioned on the left side of the collage, this arc represents the eastern boundary of the expanding blast wave. The prominent red hue corresponds to ionized hydrogen gas (H alpha emission at 656.3 nm), outlining dense, curtain-like sheets of gas viewed edge-on. The complex, curved geometry reveals localized variations in the density of the surrounding interstellar medium.

Pickering's Triangle (Fleming's Triangular Whisp / NGC 6979)

Located in the upper section and spanning toward the central background, this fainter, triangular network of delicate filaments represents a central cloud complex of the Cygnus Loop. Unlike the sharp outer arcs, Pickering’s Triangle exhibits an intricate, web-like structural diffuse emission, formed where the blast wave interacts with diffuse interstellar gas within the interior of the remnant shell". - Kurt Thrust current Director of the Jodrell Plank Observatory

The Nova in Sagitta - a classical Fe II-type nova.

 

Part of the Constellation 'Sagitta the Arrow' showing the Nova V488. The image is a compilation panorama of two stacks of images captured last night with the Observatory's Seestar S30.

Image and plate solving credit: Astrometry.net 

Google Gemini's go at identifying Nova Sagitta V488 - which Kurt believes to be wrong! As most AI software warns 'AI can make mistakes'🤣 

    

Kurt's best guess at the location of Nova V488 based on the images and charts available on the internet from credible sources 

 

"Last night from the Jodrell Plank Observatory, we managed to capture a few photons from the Cosmos. Kurt and his team were battling against the clouds and a waning gibbous Moon , which in concert did much to make imaging difficult! 

Kurt was very keen to image the current nova in the constellation Sagitta is named V488 Sagittae (also designated as Nova Sagittae 2026 or N Sge 2026).

The Seestar was the obvious choice bearing in mind it's quick set up, reasonable  field of vision and the brightness of the nova at mag 6 to 7. 

It is however very easy to mix up stars in and around the plane of the Milky Way where you are often spoilt for choice. 

We do however believe we have captured an image which shows the nova." - Joel Cairo CEO of the JPO the UKs most easterly Astronomical Observatory.

" Out of courtesy, I uploaded Kurt's best guess to Google Gemini and in response and without further comment it corrected it's annotation to agree with his. Either it just wants to please everyone or it has some way to go before 'world domination" 🤣 -Joel

Google Gemini's corrected annotation

Nova in Sagitta August 2026: Scientific Description

By Gary Gemini Coms Manager at the JPO.

V488 Sagittae (also designated Nova Sagittae 2026 / PNV J19450648+1822422) is undergoing a classic thermonuclear nova explosion.

At the centre of this cataclysmic variable system is a dense white dwarf in a tight binary orbit with a stellar companion star. Over time, the intense gravitational pull of the white dwarf pulls hydrogen-rich gas away from its donor companion, forming an accretion disk around the remnant star before settling directly onto its surface.

As this accreted layer of hydrogen accumulates on the white dwarf's surface, extreme gravitational forces compress and heat the gas. Once the base of this material reaches critical temperature and pressure thresholds (roughly 10 million Kelvin), runaway nuclear fusion is triggered.

This sudden, runaway thermonuclear blast violently ejects the outer envelope of accumulated hydrogen into space at thousands of kilometres per second. The explosion causes the progenitor system—previously an extremely dim magnitude ~21 speck—to violently brighten by hundreds of thousands of times into a bright 6th–7th magnitude optical transient before beginning its slow radiative cooling and decay phase.

Unlike a supernova, the underlying white dwarf survives the blast intact, and after the ejected shell dissipates, the mass-transfer accretion process will eventually begin anew.

Why V488 is Different from a Type 1a Supernova

V488 Sagittae (Classical Nova): This is a superficial, non-destructive surface explosion. It occurs in a close binary system where a white dwarf pulls hydrogen gas from a companion star. Once the gas pressure builds up, a thermonuclear runaway triggers on the surface, causing the system to flare up significantly in brightness before fading. The underlying white dwarf completely survives the event. 
Type Ia Supernova: This is a terminal, internal detonation. It occurs when a carbon-oxygen white dwarf accumulates so much mass that it exceeds the Chandrasekhar limit (roughly 1.44 solar masses), causing the entire star to blow itself apart and leave no remnant behind. 

Pickering's Triangle and The Cygnus Loop.

 

Pickering's Triangle and the Witches Broom Nebula. Seestar S30 EQ mode. Cropped selection from a 60 minute stack of 60 second light frames.

"Part of the Veil Nebula in Cygnus and the remnants from a supernova.  One of the joys of the Northern Hemisphere's summer and early autumn skies " - Joel Cairo CEO of the Jodrell Plank Observatory in Lowestoft, Suffolk, UK.

The Cygnus Loop: Scientific Description

By G.Gemini Coms Manager at the JPO.

The Western Veil Nebula & Pickering’s Triangle (Cygnus Loop)

This wide-field capture features two prominent components of the Cygnus Loop supernova remnant: NGC 6960 (the Western Veil, or Witch’s Broom) and Pickering’s Triangle (Simeis 3-188). Located approximately 2,400 light-years away in the constellation Cygnus, these intricate filaments trace the expanding shockwave of a core-collapse supernova that shattered a massive star roughly 10,000 to 20,000 years ago.

Arcing across the upper section, the Witch’s Broom forms a sharp, delicate shock front visually anchored by the bright foreground star 52 Cygni (mag 4.2). The ribbon displays strong colour separation created by distinct atomic transitions: rich magenta-red hues from ionized hydrogen (H alpha emission at 656.3 nm) complemented by subtle cyan filaments corresponding to doubly ionized oxygen ([O III] emission at 500.7 nm), where supersonic shocks heat the interstellar medium. Across the lower frame, Pickering's Triangle unfolds into a intricate web of braided gas threads, showcasing diffuse hydrogen emission interlaced with faint ionization boundaries.

Acquisition & Processing Details:

• Telescope/Camera: ZWO Seestar S50 (Equatorial Mode)

• Integration: 60 × 60s exposure lights (1 hour total integration)

• Gradient Correction: GraXpert

• Star Separation: StarNet GUI

• Post-Processing & Composition: Affinity Photo 2

Curiosity said Alice!

 

The Martian Vista captured by the mast-cam of the Curiosity Rover.

NASA/JPL-Caltech/MSSS

" When you make something well it does last, even in the most extreme of environments. This image taken by the Curiosity Rover on Mars at its highest elevation to date, really underlines the extreme nature of the Martian Environment. 

In a timescale of one million years the Sun will have begun to heat up as part of its ageing process. Life on Earth will eventually become impossible. In the meantime, rather than prioritising humanity's escape to Mars, we might be better to invest resources in protecting our environment and defending the one 'Million Years', which is an enormous amount of time and represents at least 100,000 future generations". - Joel Cairo CEO of the Jodrell Plank Observatory.

"I was surprised to see our sponsor's image of the Andromeda Galaxy, captured with the Seestar S30, in the September issue of Astronomy Now. Who knew the 'old boy' would get to be astronomically popular?" - Kurt Thrust current Director of Jodrell Plank Observatory.

Sometimes you find an unexpected interloper.

 

" Kurt was getting his head around an update of the Seestar App and as part of the process pointed the S30 at the Elephant's Trunk Nebula IC1396 for a couple of minutes. He then forgot all about it. When I came across the data, I noticed that the 'Elephant' had been photobombed by a meteor, possibly a Perseid straggler" - Joel Cairo CEO of the JPO the UK's most easterly Astronomical Observatory.

Comet 220P McNaught.

 

" The Seestar S30 was on 'outreach work' and was used by Kurt to image the short period comet 220P McNaught in the early hours of this morning whilst it was moving against the background of the Constellation Cetus. The comet surprised everyone this year by unexpectedly brightening in the night sky.". - Joel Cairo CEO of the Jodrell Plank Observatory.

Comet 220P McNaught: Scientific Description

By Gary Gemini Coms Manager at the JPO.

Comet 220P/McNaught is a short-period, Jupiter-family comet with an orbital period of approximately 5.51 years. First discovered by astronomer Robert H. McNaught in May 2004, its orbit is characterized by a perihelion distance of ~1.56 AU, an aphelion extending to ~4.68 AU near Jupiter's orbit, and a low orbital inclination of ~8.1°.

Morphological Features in the Exposure:

Optically Dense Coma: The image captures a highly condensed central pseudo-nucleus surrounded by an asymmetrical coma. The bluish-white hue around the nucleus stems primarily from cyanogen ($CN$) and diatomic carbon ($C_2$) radical gas emissions driven by solar ultraviolet radiation and photo-excitation.

Structural Dust Tail: 

Extending towards the upper-right quadrant, the prominent tail consists mainly of millimeter- to micrometer-sized dust grains pushed outward by solar radiation pressure along the anti-solar direction.

Outburst Morphology: to

 The pronounced brightness and extended structure visible here align with 220P's dramatic activity phases, such as the major outbursts where sublimating subterranean ices (like $CO$ or $CO_2$) violently ruptured the refractory mantle, ejecting massive plumes of dust and volatile gases.

Enlarged crop of the original stacked image.

The Universe is big, very big!

 

"The above is an annotated version of an image captured and created with the JPO's Seestar S30. 

The Seestar S30 has a field of vision of only  0.0064% of the entire celestial sphere or sky. A tiny amount in the scheme of things. 

In addition the Seestar, having an aperture of only 30mm has limited light grasp, so can only image objects down to apparent magnitude 12 to 15, dependant upon light pollution and length of exposure.

Both the above limitations, inherent to the Seestar S30, act to minimise the number of stars imaged.

The above Seestar image is estimated by AI to contain somewhere between 300 and 400 billion stars. The overwhelming majority of these stars are held within the galaxies identified in the above image. The spiral galaxy NGC 7479, the Propeller Galaxy, contains 100 to 200 billion stars alone.

The Universe is a very very big place indeed". - Kurt Thrust current Director of the Jodrell Plank Observatory.

Messier 8 reviewed in detail.

 

The Lagoon Nebula Messier 8 
Data credit: the PIRATE robotic telescope. 
Open Observatories, Open University, telescope.org.
(Rendered two ways using Affinity Photo software)

" The wonderful  Messier 8 aka the Lagoon Nebula, never rises much above our southern horizon at the Jodrell Plank Observatory. We therefore use data captured from Tenerife much further south. The Nebula is a mix of dust and ionized gas and is a home to star birth in the Milky Way."- Joel Cairo CEO of the Jodrell Plank Observatory.

Messier 8 the Lagoon Nebula: Scientific Description

By Gary Gemini Coms Manager at the JPO.

Image Analysis & Morphological Features

Captured using the PIRATE (Physics Innovations Robotic Telescope Explorer) instrument at the Observatorio del Teide, Tenerife, this wide-field frame resolves the core structural dynamics of Messier 8 (M8), a massive H II region.

The image highlights the complex interplay between photo-ionized gas, obscuring interstellar dust, and young stellar associations:

Central Ionization Zone & The Hourglass Nebula: 

At the physical center lies an intensely bright, high-surface-brightness core driven by extreme photo-ionization. Situate in here is the Hourglass Nebula, a highly turbulent sub-region sculpted by stellar winds and ionizing ultraviolet radiation primarily originating from the massive O-type supergiant Herschel 36 (visible as the bright star adjacent to the central core).

Central Ionization Zone and Hourglass Nebula

Dust Topography & Dark Nebulae: 

Sweeping lanes of cold molecular gas and opaque dust cross-cut the emission background. The prominent central dust lane—the feature historically giving M8 its "Lagoon" namesake—is clearly visible, alongside small, dense, collapsing protostellar dust clouds known as Bok globules (such as Barnard 88, 89, and 296) silhouetted against the bright ionized hydrogen background.

Open Cluster NGC 6530: 

To the east (left) of the core lies NGC 6530, an embedded, extremely young open star cluster born directly out of the nebula’s parent molecular cloud. Its hot, massive stars contribute significantly to the collective UV flux driving the illumination of the surrounding gas.

Physical & Astrophysical Attributes

Classification: Active H II Region / Emission Nebula with associated Open Star Cluster (NGC 6530).

Constellation: Sagittarius

Distance: ≈4,100 to 5,200 light-years (1.25 to 1.60 kpc) from Earth.

Physical Extent: Spans roughly 110×50 light-years (≈33×15 pc).

Excitation Mechanism: Photo-ionization driven by high-energy far-ultraviolet photons (λ<91.2 nm) emitted by massive, hot O- and B-type stars. Recombination processes in the ionized hydrogen gas generate the dominant Hα emission lines.

Stellar Population: The region serves as an active site of ongoing star formation. NGC 6530 is estimated to be only 2 to 4 million years old, housing hundreds of young, high-mass stars, protostars, and Herbig-Haro objects embedded deep within its dust lanes.

Bok globules.

Herbig-Haro objects embedded in dust clouds.

Does size really matter?

 

" The top image is of part of the Rosette Nebula in the constellation Monoceros the Unicorn. It was captured using the 16 inch (400mm.) aperture PIRATE robotic telescope located at altitude on the extinct volcano Mount Teide, Tenerife. The lower image is of all of the Rosette Nebula captured with our 30mm aperture Seestar 'smartscope' at Sea-level from the JPO in Lowestoft. Apart from the orientation they are remarkably similar in their resolution of detail.  

Clearly, the research grade telescope located under a dark sky at altitude in Tenerife has provided the better image but how much better is a matter for debate. Having access to both sets of data is definitely a bonus for the JPO imaging team and we remain grateful to Open Observatories, the Open University and telescope.org.

For astronomers who like to capture their own data and in terms of value for money, mobility and ease of use, the Seestar S30 is an incredible piece of kit for the use of beginners and seasoned astro-imagers alike!" - Joel Cairo CEO of the Jodrell Plank Observatory.

Messiers 27 and 76 on the comparative method.

 

Messier 27 'The Dumbbell Planetary Nebula  captured by Kurt Thrust from the Jodrell Plank Observatory with the 127 mm Meade 500 series apo refractor and a Canon 600d DSLR. Reprocessed data - to show finer detail in the nebulosity.

" Kurt is definitely becoming obsessive in his old age and is reprocessing more old data whilst he can. More concerning, he is showing a rather morbid interest in planetary nebulae 'the end of days' for stars of a certain size, like our own planet Earth". - Joel Cairo CEO of the JPO the UK's most easterly astronomical observatory.

Messier 27 and Messier 76: Scientific Description

By Gary Gemini Coms Manager at the JPO.

The image depicts Messier 27 (M27), commonly known as the Dumbbell Nebula—a classic, highly evolved planetary nebula situated approximately 1,200 light-years away in the constellation Vulpecula.

Technical & Physical Morphology

• Gas Ionization and Composition: The central region glows in vibrant blue-green tones, indicative of high-energy, doubly ionized oxygen ( emission around 501 nm), excited by intense ultraviolet radiation emitted from the hot central star. The outer envelope and peripheral rim show intense red and deep orange hues, corresponding to lower-ionization transitions, primarily hydrogen-alpha ( at 656 nm) and ionized nitrogen (N II).

• Structural Geometry: M27 exhibits an oblate prolate spheroidal structure tilted at a shallow angle relative to our line of sight. The characteristic "dumbbell" or "apple core" appearance is created by an equatorial concentration of denser gas (the thick central bar/waist) paired with broad polar outflows that extend outward, forming a faint outer halo.

• Microstructure and Instabilities: Detailed throughout the interior is a complex, cellular network of dark and illuminated filaments. These are cometary knots—dense globules of neutral gas and dust being ionized and eroded by high-speed stellar winds and photoevaporation driven by the central star.

Planetary Nebulae M27 on the left M76 on the right.

Comparison: M27 vs. M76 (The Little Dumbbell Nebula)

Feature	Messier 27 (Dumbbell Nebula)	Messier 76 (Little Dumbbell Nebula)
Morphological Type	Elliptical / Prolate Spheroid	True Bipolar Planetary Nebula
Viewing Angle	Pole-on to intermediate inclination	Edge-on equatorial torus
Structure	Broad, filled central volume with subtle polar caps	Distinct central bar/ring with two extended outer lobes
Stellar Dynamics	Ejected mainly by a single evolving star	Sculpted likely via interaction with a binary companion

Fate of the Sun and the Solar System

M27 provides a direct preview of the ultimate death of our Sun in roughly 5 billion years:

1. Fuel Exhaustion: Once the Sun exhausts its core hydrogen, it will expand into a Red Giant, fusing helium in shell-burning phases (Asymptotic Giant Branch stage).

2. Mass Ejection: Thermal pulses will cause the Sun to shed its outer envelope into space via stellar winds, creating a glowing shell identical to the nebula shown here.

3. Core Remnant: The exposed, superheated carbon-oxygen core will become a white dwarf (visible at the centre). Its intense UV radiation will energize the surrounding gas for ~10,000–50,000 years before the gas expands into the interstellar medium and fades away.

4. Solar System Destruction: Mercury and Venus will be engulfed; Earth will either be consumed or reduced to a scorched, lifeless rock orbiting a cooling white dwarf remnant.

" Always good to finish on an upbeat note"  - Kurt Thrust current Director of the Jodrell Plank Observatory.