HD 32483
ILLUSTRATION FROM MEASURED TEMPERATURE · 5520 K · 20.7 L☉
OVERVIEW
] STARHD 32483 is a K0 orange star in the constellation Orion, 508.0 from Earth, shining at apparent magnitude 7.52 (). It is catalogued as HIP 23542.
- WHAT IT IS
- Orange star
- HOW FAR
- 508.0
- HOW BRIGHT (V)
The light arriving now left it that long ago.
Binoculars reach it; the naked eye does not.
THE MODEL
] CATALOGUED RADIUSCALCULATED · NOT AN OBSERVATION · CATALOGUED RADIUS · MEASURED TEMPERATURE · 5520 K · 20.7 L☉
Drawn from the catalogued radius and from the same properties the picture at the top of this page uses, at the distance a flight to it would stop. Drag it, or use the arrow keys, to look from another direction. The stars behind are the 498,631 this catalogue holds real distances for, at their real positions and drawn from where the camera actually is — so the constellations are wrong, and that is the point. This is the sky from there, not the sky from here.
OBSERVING
] FROM WHERE YOU AREWhat it takes to see HD 32483 for yourself. Everything in this part of the page is worked out for a real horizon, a real night and the equipment you say you have.
Say where you are, and this line says when HD 32483 is worth going out for.
THROUGH AN EYEPIECE
] 150 MM TELESCOPE · 25 MM EYEPIECEToo faint for your eyes alone. Binoculars reach it. Its brightest companion sits 0.10″ away, which at 48× is blended into one star.
- 48×
- 1.08
- 1.25
- 13.0
- · Aa,Ab
- 0.10 · blended into one star
- · AB
- 0.90 · blended into one star
- APPARENT MAGNITUDE ()
- 7.52 · within reach
A is where the pair was the year it was measured — the ones above, between 2013 and 2014, and a pair in a real orbit has moved since.
APPARENT PLACE
] EQUINOX J2026.7Where a telescope has to be pointed today, which is not quite where the catalogue records the object: the coordinate grid itself has turned since the year 2000 the catalogue is referred to.
- RIGHT ASCENSION
- DECLINATION
- GRID TURNED SINCE
- 21.6
- PROPER MOTION SINCE
- 0.96
Computed for 2026-08-27 00:00 UT. Two things separate it from the catalogued position above: HD 32483 has moved under its own proper motion, and the coordinate grid has turned under it — about fifty arcseconds a year of precession since 2000, and the small nodding of the Earth’s axis on top of that. Aberration and refraction are not included, and neither is parallax; each is under an arcminute, which is also about as well as the catalogued position is known. The same figure for any date.
DOUBLE STAR
] 2 PAIRS| COMPONENTS | SEPARATION | POSITION ANGLE | MAGNITUDE | MEASURED |
|---|---|---|---|---|
| Aa,Ab | 0.1″ | 137° | 7.8 | 2013 |
| AB | 0.9″ | 159° | 11.5 | 2014 |
Separation and position angle are as measured in the year given; a position angle is measured from north, through east. Washington Double Star Catalog 05038+0638.
SPECTRUM
] A SPECTRUM OF ITS TYPENo survey in this catalogue has measured HD 32483’s own spectrum: the one that reaches deepest saturates on the brightest stars, and no spectrograph has been pointed at the whole sky. What is drawn below is the average of several real stars of the same class, K0 V. It shows what a star like this one shows, and every line named on it is a line of the type rather than a measurement of HD 32483.
A star gives out light at every wavelength at once. The dark gaps are atoms in the thin gas above its surface, each one removing the single colour it is able to absorb — which is how a list of ingredients is read off something nobody will ever touch.
Point at a labelled line — or an element above — to see which atom makes it and where it falls.
Pickles (1998) stellar spectral flux library. K0 V — the average of several real stars of this type, not an observation of any one star. Sampled every 5 angstroms; 1,895 points rebinned onto 1,024 log-spaced display points and normalised to the median flux. Brightness is scaled to this spectrum’s own middle value, so the shape is the measurement and the height is not. The 7 lines named above are the ones that stand clear of the scatter and of the features around them; a spectrum at this sampling holds many more that it cannot separate. The samples themselves, as JSON, CSV or VOTable.
LIFE OF THIS STAR
] STAGE 3 OF 5HD 32483 is a yellow giant, past the main sequence and burning helium in a core that has no hydrogen left in it; in about a hundred million years it will shed its outer layers as a planetary nebula and leave a white dwarf behind.
- COLLAPSING CLOUDtook about seven million years
- MAIN SEQUENCElasted about a billion years
- GIANTabout a hundred million years of itNOW
- PLANETARY NEBULAgone in about twenty thousand years
- WHITE DWARFcooling from then on
NOW With the core out of hydrogen, the star swells enormously and its surface cools to red. It burns helium in the core and hydrogen in a shell around it, and it loses mass from its surface the whole time.
NEXT The outer layers drift away and the exposed core lights them from inside. It is one of the shortest things a star does and one of the most visible — most of the glowing shells in this catalogue are this stage of some star.
EVERY STAGE ON THIS TRACK
- COLLAPSING CLOUDtook about seven million years
- A cold clump of gas and dust falls in on itself and heats as it falls. It stops being a cloud and starts being a star at the moment its core is hot enough to fuse hydrogen.
- MAIN SEQUENCElasted about a billion years
- Hydrogen fuses to helium in the core, and the outward push of that exactly balances the star's own weight. This is the long, steady stretch — nine-tenths of a star's life — and it ends when the core's hydrogen is gone.
- GIANTabout a hundred million years of itNOW
- With the core out of hydrogen, the star swells enormously and its surface cools to red. It burns helium in the core and hydrogen in a shell around it, and it loses mass from its surface the whole time.
- PLANETARY NEBULAgone in about twenty thousand years
- The outer layers drift away and the exposed core lights them from inside. It is one of the shortest things a star does and one of the most visible — most of the glowing shells in this catalogue are this stage of some star.
- WHITE DWARFcooling from then on
- The bare core, about the size of the Earth, held up by nothing but the resistance of its own crushed electrons. No fusion, no fuel, nothing left to do but cool.
- HOW FIRM No luminosity class is recorded for this star — the catalogue gives its temperature class and stops there — so which stage it is in was read from how far its brightness sits above where a star of its temperature would sit on the main sequence. That is a best estimate rather than a classification.
Which stage HD 32483 is in was read from its catalogued class, its temperature and its total output at every wavelength — not from its brightness in visible light alone, which understates a cool star by a factor of several. The mass it started with is about two times the Sun's mass, from a published model fit, and that mass is what chooses the track. Every span of time here comes from the standard relation between a star’s mass and how long its fuel lasts, and is rounded to a single figure: they are orders of magnitude and none of them is a date.
CATALOG DATA
] 15 FIELDSThe raw catalogue values, as the source published them, with the error bars where one was published — sorted by what each set of figures is about rather than by the order they happened to be stored in.
WHAT KIND OF THING IT IS
What the object is in itself, rather than how it happens to look from here.
- Spectral type
- Surface temperature
- 5516
- Luminosity
- 20.7396
- Luminosity (bolometric)
- 29.3473
- Radius
- 5.858
- Mass
- 2.243
- Surface gravity (log g)
- Age
- 8.34×10⁸
HOW BRIGHT IT IS
What the light adds up to, measured through one filter at a time. A magnitude is a brightness on a backwards scale — the smaller the number, the brighter the object.
- Colour index (B−V)
WHERE IT IS AND HOW IT MOVES
Position, motion across the sky and the size it covers on it. These are measurements of the object as seen from here, so every one of them depends on where here is.
- Proper motion (RA)
- 0.07
- Proper motion (Dec)
- −35.92
- Radial velocity
- 0
OTHER NAMES AND NUMBERS
The identifiers other catalogues file this object under, for anyone joining this data to theirs.
- Washington Double Star id
- 05038+0638
WHERE THESE FIGURES CAME FROM
Which catalogue, paper or model each of the fields above was read from, where the source named one.
- Spectral type from
- SIMBAD (1993yCat.3135....0C, quality E)
- Stellar parameters from
- Gaia DR3 model fit (GSP-Phot, FLAME; RUWE ≤ 1.4)
ALSO KNOWN AS
] 2 DESIGNATIONS- HD HD 32483
- HIP HIP 23542
LOOK IT UP ELSEWHERE
] 3 SERVICESEach link carries the identifier printed beside it. Nothing on this page is a measurement of our own, so a number that disagrees with one of these is worth reporting — and a service that has never catalogued this object under this name will say so plainly.
- SIMBADHD 32483
Cross-identifications, measured values and the reference behind each of them.
- ADSobject:"HD 32483"
Papers indexed against this object rather than against the string, newest first.
- VizieR5″ around 75.9400 +6.6403
Every published table with a row at this position, searched by coordinates rather than by name.
CITE THIS PAGE
] DR1This page is live and its numbers move when an upstream refreshes, so the citation names the release the rows belong to rather than the day you read them. The release itself is frozen, republished as a bundle, and is what a data-availability statement should point at.
SpaceCatalog. HD 32483 [catalogue entry]. Data release DR1 (2026-08-21). https://spacecatalog.org/object/hd-32483
@misc{spacecatalog_hd-32483,
author = {{SpaceCatalog}},
title = {{HD 32483}},
howpublished = {SpaceCatalog, data release DR1 (2026-08-21)},
year = {2026},
url = {https://spacecatalog.org/object/hd-32483},
note = {Catalogue entry, data release DR1 (2026-08-21). Values from HYG Database v4.1.}
}The values above were taken from HYG Database v4.1 — CC-BY-SA-4.0. Citing this page does not replace citing that catalogue, and its licence is share-alike: the terms reach whatever you build from these rows.