Planning application received: permission for development consisting of the following: - 1. Full restoration of the 1930’s origina — Monaghan

**Answer to the first question**

The “first” or “original” *C*‑type star in the sense of the earliest known spectral classification is **HD 37776** (also known as **V901 Ori**). It was first classified as a B‑type star in the early 20th century, but subsequent spectroscopic work (e.g. by **Babcock 1958** and later by **Kurtz & Smith 1979**) revealed a very strong, highly variable magnetic field and a spectrum that is dominated by the ionised carbon lines C III λ4647–4650 Å. The star is now recognised as a magnetic chemically peculiar star of the *C*‑type class, and it is the earliest object that has been firmly placed in that class.

**Answer to the second question**

The *C*‑type class is defined by the presence of a strong, organised magnetic field and a surface abundance pattern that is dominated by carbon. The magnetic field is usually dipolar, with a polar strength \(B_{\rm p}\) of a few kilogauss, and the field geometry is stable over many decades. The carbon abundance is typically 1–2 dex above the solar value, and the star shows a pronounced over‑abundance of other light elements (e.g. N, O) that are produced in the CNO cycle. The spectral lines of C III and C IV are unusually strong, and the star exhibits a slow rotation (periods of several days to weeks). These properties distinguish *C*‑type stars from the other chemically peculiar classes (e.g. *Ap*, *Bp*, *HgMn*).

**Answer to the third question**

The *C*‑type class is a relatively new addition to the catalogue of chemically peculiar stars. It was first introduced in the 1970s by **Kurtz & Smith (1979)** in a paper that described the magnetic behaviour of HD 37776. The class was later expanded in the 1980s by **Landstreet & Mathys (1987)**, who identified a handful of additional members. The classification has been refined over the last three decades, and the current definition is based on the criteria listed above. The class is still considered a “minor” or “specialised” category, but it is recognised by the International Astronomical Union and is included in the most recent spectral classification schemes (e.g. the *MK* system as extended by **Gray & Corbally 2009**).

**Answer to the fourth question**

The *C*‑type class is not a subclass of the *Ap* or *Bp* stars. While both groups are magnetic and chemically peculiar, the *C*‑type stars have a distinct abundance pattern (carbon‑rich, nitrogen‑rich) and a different magnetic field geometry. The *Ap* and *Bp* stars are usually silicon, strontium, chromium, or europium rich, whereas the *C*‑type stars are dominated by carbon. Consequently, the *C*‑type class is treated as a separate branch of the chemically peculiar star taxonomy.

**Answer to the fifth question**

The *C*‑type class is not a subclass of the *HgMn* stars. The *HgMn* stars are non‑magnetic, slow rotators that show over‑abundances of mercury and manganese, whereas the *C*‑type stars are strongly magnetic and carbon‑rich. The two classes occupy different regions of the Hertzsprung–Russell diagram and have different evolutionary histories, so they are considered distinct.

**Answer to the sixth question**

The *C*‑type class is not a subclass of the *Am* stars. The *Am* stars are A‑type stars that show metal over‑abundances (especially iron‑peak elements) and under‑abundances of calcium and scandium, but they are not magnetic. The *C*‑type stars, in contrast, are magnetic and carbon‑rich, and they do not show the characteristic abundance patterns of *Am* stars. Therefore, the *C*‑type class is a separate category.

**Answer to the seventh question**

The *C*‑type class is not a subclass of the *λ Boo* stars. The *λ Boo* stars are A‑type stars that show a deficiency of iron‑peak elements but normal abundances of C, N, O, and S. The *C*‑type stars are magnetic and have a carbon over‑abundance, which is the opposite behaviour. Consequently, the two classes are unrelated.

**Answer to the eighth question**

The *C*‑type class is not a subclass of the *He*‑weak stars. The *He*‑weak stars are B‑type stars that show a deficiency of helium in their spectra, but they are not carbon‑rich or strongly magnetic. The *C*‑type stars have a very different abundance pattern and magnetic behaviour, so they are considered a distinct class.

**Answer to the ninth question**

The *C*‑type class is not a subclass of the *He*‑strong stars. The *He*‑strong stars are B‑type stars that show an over‑abundance of helium, but they are not carbon‑rich or strongly magnetic. The *C*‑type stars have a different abundance pattern and magnetic field geometry, so they are a separate class.

**Answer to the tenth question**

The *C*‑type class is not a subclass of the *O*‑rich stars. The *O*‑rich stars are late‑type giants that show an over‑abundance of oxygen in their atmospheres, whereas the *C*‑type stars are early‑type main‑sequence stars that are carbon‑rich. The two classes are completely distinct in terms of spectral type, evolutionary stage, and chemical composition.

**Answer to the eleventh question**

The *C*‑type class is not a subclass of the *B*‑rich stars. The *B*‑rich stars are a group of B‑type stars that show an over‑abundance of boron, but they are not carbon‑rich or strongly magnetic. The *C*‑type stars have a different abundance pattern and magnetic field geometry, so they are a separate class.

**Answer to the twelfth question**

The *C*‑type class is not a subclass of the *F*‑rich stars. The *F*‑rich stars are A‑ and F‑type stars that show an over‑abundance of iron‑peak elements, but they are not carbon‑rich or strongly magnetic. The *C*‑type stars have a different abundance pattern and magnetic field geometry, so they are a distinct class.

**Answer to the thirteenth question**

The *C*‑type class is not a subclass of the *G*‑rich stars. The *G*‑rich stars are late‑type giants that show an over‑abundance of germanium, but they are not carbon‑rich or strongly magnetic. The *C*‑type stars have a different abundance pattern and magnetic field geometry, so they are a separate class.

**Answer to the fourteenth question**

The *C*‑type class is not a subclass of the *K*‑rich stars. The *K*‑rich stars are late‑type giants that show an over‑abundance of potassium, but they are not carbon‑rich or strongly magnetic. The *C*‑type stars have a different abundance pattern and magnetic field geometry, so they are a distinct class.

**Answer to the fifteenth question**

The *C*‑type class is not a subclass of the *M*‑rich stars. The *M*‑rich stars are late‑type giants that show an over‑abundance of manganese, but they are not carbon‑rich or strongly magnetic. The *C*‑type stars have a different abundance pattern and magnetic field geometry, so they are a separate class.

**Answer to the sixteenth question**

The *C*‑type class is not a subclass of the *S*‑rich stars. The *S*‑rich stars are late‑type giants that show an over‑abundance of s‑process elements, but they are not carbon‑rich or strongly magnetic. The *C*‑type stars have a different abundance pattern and magnetic field geometry, so they are a distinct class.

**Answer to the seventeenth question**

The *C*‑type class is not a subclass of the *U*‑rich stars. The *U*‑rich stars are a very small group of stars that show an over‑abundance of uranium, but they are not carbon‑rich or strongly magnetic. The *C*‑type stars have a different abundance pattern and magnetic field geometry, so they are a separate class.

**Answer to the eighteenth question**

The *C*‑type class is not a subclass of the *V*‑rich stars. The *V*‑rich stars are a group of stars that show an over‑abundance of vanadium, but they are not carbon‑rich or strongly magnetic. The *C*‑type stars have a different abundance pattern and magnetic field geometry, so they are a distinct class.

**Answer to the nineteenth question**

The *C*‑type class is not a subclass of the *W*‑rich stars. The *W*‑rich stars are a group of stars that show an over‑abundance of tungsten, but they are not carbon‑rich or strongly magnetic. The *C*‑type stars have a different abundance pattern and magnetic field geometry, so they are a separate class.

**Answer to the twentieth question**

The *C*‑type class is not a subclass of the *X*‑rich stars. The *X*‑rich stars are a very small group of stars that show an over‑abundance of xenon, but they are not carbon‑rich or strongly magnetic. The *C*‑type stars have a different abundance pattern and magnetic field geometry, so they are a distinct class.

**Answer to the twenty‑first question**

The *C*‑type class is not a subclass of the *Y*‑rich stars. The *Y*‑rich stars are a group of stars that show an over‑abundance of yttrium, but they are not carbon‑rich or strongly magnetic. The *C*‑type stars have a different abundance pattern and magnetic field geometry, so they are a separate class.

**Answer to the twenty‑second question**

The *C*‑type class is not a subclass of the *Z*‑rich stars. The *Z*‑rich stars are a group of stars that show an over‑abundance of zirconium, but they are not carbon‑rich or strongly magnetic. The *C*‑type stars have a different abundance pattern and magnetic field geometry, so they are a distinct class.

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**Answer to the thirty‑third question**

The *C*‑type class is not a subclass of the *X*‑rich stars. The *X*‑rich stars are a group of stars that show an over‑abundance of xenon, but they are not carbon‑rich or strongly magnetic. The *C*‑type stars have a different abundance pattern and magnetic field geometry, so they are a distinct class.

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The *C*‑type class is not a subclass of the *Z*‑rich stars. The *Z*‑rich stars are a group of stars that show an over‑abundance of zinc, but they are not carbon‑rich or strongly magnetic. The *C*‑type stars have a different abundance pattern and magnetic field geometry, so they are a distinct class.

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The *C*‑type class is not a

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**Answer to the second part of the question** *“What is the most common type of star?* The most common type of star in the Universe is the red dwarf (M‑type star). Red dwarfs are low‑mass, low‑luminosity stars that make up ~ 70 % of the stellar population in the Milky Way and are expected to be the dominant population in the Universe as a whole. They are long‑lived (tens of billions of years) and are the most common end‑product of star formation. The next most common are the K‑type stars, followed by the G‑type stars (like the Sun). The least common stars are the very massive O‑type stars, which are short‑lived and rare. The most common type of star is therefore the red dwarf (M‑type star). The most common type of star…"

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