SX Arietis variable
Let an agent explain SX Arietis variables by mechanism, properties and relation to other magnetic variables, and support observation and data access.
Bundle → Layer → Finding → Questions Filled
4 bundles · 8 layers · 8 findings · 16 questions
Mechanism Why they vary.
Rotation
Rotational modulation.
Rotation
Rotational modulation.
- How do chemically peculiar regions and rotation produce the variability? definition
- What is the rotation period? measurement
Magnetic
Magnetic fields.
Magnetic
Magnetic fields.
- How strong are the magnetic fields, and how are they measured? measurement
- How do they shape the surface abundances? definition
Properties What they are.
Star
Stellar properties.
Star
Stellar properties.
- What are the spectral type, temperature and peculiarities of this star? provenance
- How large is the amplitude? measurement
Classify
Classification.
Classify
Classification.
- Is the star an SX Arietis or alpha2 CVn variable, and which criteria decide? definition
- Which catalogue records it? provenance
Science Wider relevance.
Evolution
Origins of fields.
Evolution
Origins of fields.
- Where do the magnetic fields of these stars come from, according to current theories? provenance
- How do they evolve? provenance
Compare
Other rotating variables.
Compare
Comparison.
- How do SX Arietis stars compare with BY Draconis and alpha2 CVn stars? definition
- What do they have in common? definition
Observing Data.
Data
Light curves.
Data
Light curves.
- Where can light curves and spectra for this star be found? provenance
- Which surveys observe it? provenance
Amateur
Observing.
Amateur
Amateur observing.
- Can amateurs detect the small variations with photometry? boundary
- How can observations be reported? action
Classifiers Filled
- Family
- Thing Registry
- Category
- Physical world and living systems
- Entry kind
- thing
- Plane
- PHY
- Domain
- PHY.SPC
What it is Filled
A class of rotating variable stars, mainly hot main-sequence stars of spectral types B0 to B9 with strong magnetic fields, whose brightness and spectral line strengths vary with rotation as chemically peculiar surface regions rotate in and out of view, with periods of about one day; the prototype is SX Arietis and they are the hotter analogues of alpha2 Canum Venaticorum variables.
Why it exists Filled
Let an agent explain SX Arietis variables by mechanism, properties and relation to other magnetic variables, and support observation and data access.
Distinguishing features Filled
- Rotational modulation
- Strong magnetic fields
- Hot B-type stars
- Chemically peculiar surfaces
What robots and AI may and may not do Filled
Must not
- Misclassify a star in a catalogue without evidence.
- Publish other observers' data without credit.
Only with a human decision
- Submitting a new classification to a variable star catalogue.
May
- Describe SX Arietis variables and list known members from catalogues.
- Process photometric data the agent is authorized to analyse.
Moral aspects Filled
- Astronomy relies on shared data and fair credit, including amateur observers.
- Catalogue errors persist and mislead later work.
Who is affected
- Researchers
- Amateur observers
Owners Filled
Steward
Nobody owns the stars; variable star catalogues record them.
Master systems
- General Catalogue of Variable Stars
- Astronomical object databases
Links to other meta-models Filled
parent
- Q2168098 - registry parent class
related
- rotating variable star - category
- SX Arietis - prototype
- BY Draconis variable - other rotating variable
- W Virginis variable - other variable class
What else AI and robots need to interact with it Filled
Identity and identifiers required Filled
- Vercy registry: vr.tr.sx-arietis-variable
- Wikidata: Q1392904 (https://www.wikidata.org/wiki/Q1392904)
- GCVS type: SXARI variable star type
Direct properties required Filled
- Rotation period: day - Recurring brightness or spectral variations provide an estimate of the rotation period, commonly on the order of a day.
- Effective temperature: K - Effective temperature is inferred by comparing observed spectra and flux distributions with stellar atmosphere models.
- Mean longitudinal magnetic field: gauss - Spectropolarimetry estimates the visible surface average of the magnetic field component along the line of sight.
Recognition required Filled
- B-type stars with helium or silicon peculiarities
- Periods near one day
- BY Draconis variables are cool spotted stars
- Hot blue stars with small periodic brightness variations.
Capabilities and actions required Filled
- describe the rotational modulation mechanism
- identify SX Arietis star properties
- relate them to alpha2 CVn and BY Draconis stars
- find light curves and catalogues
Hazards and failure modes required Filled
- Confusing rotational and pulsational variability
- Misclassifying as eclipsing binaries
Standards and interfaces required Filled
- General Catalogue of Variable Stars classification
Context of use required Filled
- Stellar astrophysics and variable star observing.
- helium-strong SX Arietis stars
- helium-weak variants
- related alpha2 CVn variables (cooler)
Sources Filled
- Wikidata item Q1392904: SX Arietis variable - identity and sense of the item
- Wikipedia: SX Arietis variable - general description of the item
Open questions
- Should alpha2 CVn variables be linked or merged?
- How should magnetic field data be linked?
- How should survey data be linked?
Machine files
Provenance
thing registry research (pass 2) · unreviewed
Built from: models/things/publications/thing-q1392904/spec.json