Wolf-Rayet classes ...
- Thread starter anikaiful
- Start date
There are subclasses of them. So far as I know there's:
W (handplaced Wolf-Rayet)
WC
WN
WNC
WO
W (handplaced Wolf-Rayet)
WC
WN
WNC
WO
Thanks. Might conclude that the rest of the types are also present then
- had included those in my project's database already ("just in case"), but wasn't sure if they were needed to exist there or not On that note though, about white dwarves... I know DA and DC are around, but what about the rest?
Last edited:
Again so far as I know (think there could be more):
D (handplaced White Dwarf)
DA
DAB
DAV
DB
DC
DCV
DQ
(would guess there might be DBV, DQV)
Posting on lunch break - if you like I can find the descriptive text from the system map for each of them later.
D (handplaced White Dwarf)
DA
DAB
DAV
DB
DC
DCV
DQ
(would guess there might be DBV, DQV)
Posting on lunch break
- if you like I can find the descriptive text from the system map for each of them later.
Last edited:
Snipped from the following link:http://www.gutenberg.us/articles/morgan-keenan_spectral_classification#cite_note-WR-45
Though not all of the spectral classifications hold for each star type/name in ED as has been demonstrated in Jackie's thread on the decoding the Stellar Forge.
CLASS W: WOLF–RAYET
Class W or WR represents the Wolf–Rayet stars, notably unusual since they have mostly helium in their atmospheres instead of hydrogen. They are thought to mostly be dying supergiants with their hydrogen layers blown away by stellar winds, thereby directly exposing their hot helium shells. Class W is further divided into subclasses according to the dominance of nitrogen and carbon emission lines in their spectra (and outer layers).
WR spectra range is listed below.
Example: R136a1 (WN5h)Example: Gamma2 Velorum A (WC8)Example: WR93B (WO3)
Ziljan again: the layers of a star during the late giant stages are like the layers of an onion, with various masses of fuel burning via different chains nuclear chemistry. A basic cross section looks something like this, but you have to imagine various outer layers being blown off in succession exposing the inner layers of the "onion" as each fuel source runs out (of course, once it reaches an iron core, the game of musical chairs is over, and Bam!! it's supernova time):
WHITE DWARF CLASSIFICATIONS
The class D (for Degenerate) is the modern classification used for white dwarfs – low-mass stars that are no longer undergoing nuclear fusion and have shrunk to planetary size, slowly cooling down. Class D is further divided into spectral types DA, DB, DC, DO, DQ, DX, and DZ. The letters are not related to the letters used in the classification of other stars, but instead indicate the composition of the white dwarf's visible outer layer or atmosphere.
Examples: Sirius B (DA2), Procyon B (DA4), Van Maanen's star (DZ7)The white dwarf types are as follows:
Two or more of the type letters may be used to indicate a white dwarf which displays more than one of the spectral features above. Also, the letter V is used to indicate a variable white dwarf.
Extended white dwarf spectral types:
Though not all of the spectral classifications hold for each star type/name in ED as has been demonstrated in Jackie's thread on the decoding the Stellar Forge.
CLASS W: WOLF–RAYET
Class W or WR represents the Wolf–Rayet stars, notably unusual since they have mostly helium in their atmospheres instead of hydrogen. They are thought to mostly be dying supergiants with their hydrogen layers blown away by stellar winds, thereby directly exposing their hot helium shells. Class W is further divided into subclasses according to the dominance of nitrogen and carbon emission lines in their spectra (and outer layers).
WR spectra range is listed below.
- WN, spectrum dominated by NitrogenIII-V and HeliumI-II lines
- WNE (WN2 to WN5 with some WN6), hotter or "early"
- WNL (WN7 to WN9 with some WN6), cooler or "late"
- Extended WN classes WN10 and WN11 sometimes used for the Ofpe/WN9 stars
- h tag used (e.g. WN9h) for WR with hydrogen emission and ha (e.g. WN6ha) for both hydrogen emission and absorption
- WN/C, WN stars plus strong CarbonIV lines, intermediate between WN and WC stars
- WC, spectrum with strong CarbonII-IV lines
- WCE (WC4 to WC6), hotter or "early"
- WCL (WC7 to WC9), cooler or "late"
- WO (WO1 to WO4), strong OxygenVI lines, extremely rare
Example: R136a1 (WN5h)Example: Gamma2 Velorum A (WC8)Example: WR93B (WO3)
Ziljan again: the layers of a star during the late giant stages are like the layers of an onion, with various masses of fuel burning via different chains nuclear chemistry. A basic cross section looks something like this, but you have to imagine various outer layers being blown off in succession exposing the inner layers of the "onion" as each fuel source runs out (of course, once it reaches an iron core, the game of musical chairs is over, and Bam!! it's supernova time):
WHITE DWARF CLASSIFICATIONS
The class D (for Degenerate) is the modern classification used for white dwarfs – low-mass stars that are no longer undergoing nuclear fusion and have shrunk to planetary size, slowly cooling down. Class D is further divided into spectral types DA, DB, DC, DO, DQ, DX, and DZ. The letters are not related to the letters used in the classification of other stars, but instead indicate the composition of the white dwarf's visible outer layer or atmosphere.
Examples: Sirius B (DA2), Procyon B (DA4), Van Maanen's star (DZ7)The white dwarf types are as follows:
- DA: a hydrogen-rich atmosphere or outer layer, indicated by strong Balmer hydrogen spectral lines.
- DB: a helium-rich atmosphere, indicated by neutral helium, He I, spectral lines.
- DO: a helium-rich atmosphere, indicated by ionized helium, He II, spectral lines.
- DQ: a carbon-rich atmosphere, indicated by atomic or molecular carbon lines.
- DZ: a metal-rich atmosphere, indicated by metal spectral lines (a merger of the obsolete white dwarf spectral types, DG, DK and DM).
- DC: no strong spectral lines indicating one of the above categories.
- DX: spectral lines are insufficiently clear to classify into one of the above categories.
Two or more of the type letters may be used to indicate a white dwarf which displays more than one of the spectral features above. Also, the letter V is used to indicate a variable white dwarf.
Extended white dwarf spectral types:
- DAB: a hydrogen- and helium-rich white dwarf displaying neutral helium lines.
- DAO: a hydrogen- and helium-rich white dwarf displaying ionized helium lines.
- DAZ: a hydrogen-rich metallic white dwarf.
- DBZ: a helium-rich metallic white dwarf.
- DAV or ZZ Ceti: a hydrogen-rich pulsating white dwarf.
- DBV or V777 Her: a helium-rich pulsating white dwarf.
- GW Vir, sometimes divided into DOV and PNNV: a hot helium-rich pulsating white dwarf (or pre-white dwarf.) These stars are generally PG 1159 stars, although some authors also include non-PG 1159 stars in this class.
- DCV or Gliese 86 B: a cool helium-rich white dwarf.
Last edited:
D
White Dwarf stars are stellar remnants. Nuclear fusion has now ceased, and in the absence of radiation pressure the core has collapsed to a tiny fraction of the diameter of the original star, heating it up greatly before it begins its slow cooling down phase. Surface temepratures are usually between 8,000 K and 40,000 K so these stellar remnants are blue white.
DA
(as D, plus: )
Class DA stars are white dwarf stars with a hydrogen rich atmosphere.
DAV
(as D, plus: )
DAV class stars are also known as pulsating white dwarfs as their luminosity changes according to non-radial gravity waves within the star. They have hydrogen rich atmospheres.
DAB
(as D, plus: )
Class DAB stars are white dwarf type stars with hydrogen and helium rich atmospheres and neutral helium emission lines.
DB
(as D, plus: )
Class DB stars are white dwarf sub-types with a helium rich atmosphere with neutral helium emission lines.
DC
(as D)
DCV
(as D, plus: )
Class DCV stars are white dwarfs with varying luminosity.
DQ
(as D, plus: )
Class DQ stars are white dwarfs with a carbon rich atmosphere.
White Dwarf stars are stellar remnants. Nuclear fusion has now ceased, and in the absence of radiation pressure the core has collapsed to a tiny fraction of the diameter of the original star, heating it up greatly before it begins its slow cooling down phase. Surface temepratures are usually between 8,000 K and 40,000 K so these stellar remnants are blue white.
DA
(as D, plus: )
Class DA stars are white dwarf stars with a hydrogen rich atmosphere.
DAV
(as D, plus: )
DAV class stars are also known as pulsating white dwarfs as their luminosity changes according to non-radial gravity waves within the star. They have hydrogen rich atmospheres.
DAB
(as D, plus: )
Class DAB stars are white dwarf type stars with hydrogen and helium rich atmospheres and neutral helium emission lines.
DB
(as D, plus: )
Class DB stars are white dwarf sub-types with a helium rich atmosphere with neutral helium emission lines.
DC
(as D)
DCV
(as D, plus: )
Class DCV stars are white dwarfs with varying luminosity.
DQ
(as D, plus: )
Class DQ stars are white dwarfs with a carbon rich atmosphere.
Last edited:
Nice! Thank you
Very welcome
Are these from in game system map descriptions? That would be awesome if so.
Last edited:
Yeah those are the system map descriptions. I've got a feeling I've seen a DZ somewhere in the Bubble but can't remember where...
Nice!!! Glad to see that Frontier is this detailed oriented. Looking forward to any system map updates they might have in the future. Especially regarding magnetic field strength, with in game effects of course. Flare Stars, Starquakes, Magnetars, pulsars, gamma ray bursts, etc. Along with shield/hull damage and module malfunctions galore
Would also be nice if they included metallicity. You know how I feel about that, lol.
Last edited:
It would be a nice touch by frontier to make use of the extreme properties of some stellar objects to make exploration a bit more dangerous/colorfull.
- I would expect that standing close to a WR/O star/strong X ray source would ablate shields / hull even in SC.
- Neutrons stars and BH with an accretion disk should be dangerous radiation sources
- Neutron stars and magnetars have huge magnetic fields. You could put cosmetic effects such as the HUD going haywire close to such objects.
- Being close to a Neutron star or BH should produce cracking and moaning sounds in the ship, like above a high G world. Maybe damge things a bit also
It would be a nice touch by frontier to make use of the extreme properties of some stellar objects to make exploration a bit more dangerous/colorfull.
- I would expect that standing close to a WR/O star/strong X ray source would ablate shields / hull even in SC.
- Neutrons stars and BH with an accretion disk should be dangerous radiation sources
- Neutron stars and magnetars have huge magnetic fields. You could put cosmetic effects such as the HUD going haywire close to such objects.
- Being close to a Neutron star or BH should produce cracking and moaning sounds in the ship, like above a high G world. Maybe damge things a bit also
Hopefully Frontier are reading this somewhere and nodding/smiling secretively!