V765 Cas
ILLUSTRATION FROM MEASURED TEMPERATURE · 16 500 K · VARIABLE, MAG 10.59–10.99 · PERIOD 1.716 DAYS · PULSE COMPRESSED
OVERVIEW
STARV765 Cas is a white star in the constellation Cassiopeia, shining at apparent magnitude 10.69 (). Other catalogues list it as HIP 6171.
- WHAT IT IS
- White star
- HOW BRIGHT (V)
A small telescope reaches it.
OBSERVING
FROM WHERE YOU AREWhat it takes to see V765 Cas 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 V765 Cas is worth going out for.
THROUGH AN EYEPIECE
150 MM TELESCOPE · 25 MM EYEPIECEOut of reach of binoculars; a 150 mm telescope reaches it. It will be a point of light in anything: a star is far enough away that no aperture on Earth gives it a width, and all the equipment changes is how easily you find it.
- 48×
- 1.08
- 1.25
- 13.0
- APPARENT MAGNITUDE ()
- 10.69 · within reach
APPARENT PLACE
EQUINOX J2026.8Where 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
- 15.9
- PROPER MOTION SINCE
- 0.03
Computed for 2026-10-25 00:00 UT. Two things separate it from the catalogued position above: V765 Cas 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. The catalogue it came from publishes no error for that position, so nothing here says how far this arithmetic can be trusted — the digits above are as precise as the place they were computed from, and no more. Aberration, parallax and refraction are left out. Aberration swings every position by up to twenty arcseconds over a year; parallax stays under an arcsecond for all but the nearest stars; refraction is nothing overhead and about half a degree at the horizon, where it answers to the air, not the sky. The same figure for any date.
VARIABILITY
ALGOL-TYPE ECLIPSING BINARY- RANGE, AS SAMPLED
- 10.59 – 10.99
- PERIOD
- 1.71628 days (41.2 h)
- PHASE
- 0.614 ± 0.012
- NEXT MINIMUM
- 2026-10-25 15:53 UT---------- --:-- your time
- THEN
- 2026-10-27 09:04 UT---------- --:-- your time
- THEN
- 2026-10-29 02:16 UT---------- --:-- your time
Computed for 2026-10-25 00:00 UT. A phase of zero is minimum light, and V765 Cas was last there 25.3 h before that. The ± is what the published elements can still promise: 4,033 cycles have gone by since the epoch they were measured at, and the last digit of the period compounds over every one of them — 29 min by now. It is the precision of the published figures rather than an error bar the catalogue supplied, so where that catalogue has marked a period doubtful the real spread is wider — and it does not contain the star. A binary with a third body in the system, or a pulsator whose period is slowly changing, walks away from a straight-line ephemeris by an amount only observation settles. Times are corrected for where the Earth is in its orbit, which is worth up to 8.3 minutes — the light of a star reaches us that much earlier in one season than the other, and an epoch measured a century ago has the same correction in it.
The range is the spread the Hipparcos satellite measured, converted to the visual scale. It is approximate: the satellite sampled the star on a schedule of its own, and where a star spends little of its cycle at an extreme — the floor of an eclipse, most obviously — the sampling can miss it altogether. The classification, the period and the epoch are the General Catalogue of Variable Stars’s. The phase at any instant.
LIFE OF THIS STAR
STAGE 2 OF 5V765 Cas is a blue-white star on the main sequence, fusing hydrogen in its core — about twenty million years of it in all — and when that hydrogen is gone it will swell into a supergiant, and end by exploding as a supernova and leaving a neutron star.
- COLLAPSING CLOUDtook about a hundred thousand years
- MAIN SEQUENCEabout twenty million years in allNOW
- SUPERGIANTabout two million years of it, when it comes
- SUPERNOVAbright for weeks, over in a second
- NEUTRON STARfor the rest of time
NOW 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.
NEXT The same swelling, on a star heavy enough to keep going: helium, then carbon, then a run of heavier elements each burning faster than the last, until the core is iron and fusion can release nothing more.
EVERY STAGE ON THIS TRACK
- COLLAPSING CLOUDtook about a hundred thousand 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 SEQUENCEabout twenty million years in allNOW
- 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.
- SUPERGIANTabout two million years of it, when it comes
- The same swelling, on a star heavy enough to keep going: helium, then carbon, then a run of heavier elements each burning faster than the last, until the core is iron and fusion can release nothing more.
- SUPERNOVAbright for weeks, over in a second
- The iron core collapses in about a second and the rest of the star is thrown off at a tenth of the speed of light. For a few weeks it outshines the galaxy it is in.
- NEUTRON STARfor the rest of time
- What is left of the core: a couple of solar masses in a ball the width of a city, so dense that its protons and electrons have been pressed into neutrons.
- 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.
- ALSO No mass has been measured for this star. The figure above is inferred from its temperature by way of the main-sequence relation between the two, which is tight enough to be worth stating and is still an inference.
Which stage V765 Cas 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 ten times the Sun's mass, from its luminosity, 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, 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.
- Surface temperature
- 16 477
- Radius
- 9.721
- Surface gravity (log g)
- Variability
- Algol-type eclipsing binary
- Variability type ()
- EA
- Variability period
- 1.71628
- Reference epoch ()
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)
- Variable magnitude, brightest
- Variable magnitude, faintest
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)
- −0.52
- Proper motion (Dec)
- −1.17
- 0
OTHER NAMES AND NUMBERS
The identifiers other catalogues file this object under, for anyone joining this data to theirs.
- Variable-star designation
- V765 Cas
WHERE THESE FIGURES CAME FROM
Which catalogue, paper or model each of the fields above was read from, where the source named one.
- Stellar parameters from
- Gaia DR3 model fit (GSP-Phot, FLAME; RUWE ≤ 1.4) — low confidence: above 7,500 GSP-Phot's temperature and extinction are degenerate
ALSO KNOWN AS
2 DESIGNATIONS- HIP HIP 6171
- Variable star V765 Cas
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.
- SIMBADHIP 6171
Cross-identifications, measured values and the reference behind each of them.
- ADSobject:"HIP 6171"
Papers indexed against this object rather than against the string, newest first.
- VizieR5″ around 19.7877 +58.2906
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. V765 Cas [catalogue entry]. Data release DR1 (2026-08-21). https://spacecatalog.org/object/hip-6171
@misc{spacecatalog_hip-6171,
author = {{SpaceCatalog}},
title = {{V765 Cas}},
howpublished = {SpaceCatalog, data release DR1 (2026-08-21)},
year = {2026},
url = {https://spacecatalog.org/object/hip-6171},
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.
That catalogue asks for this acknowledgement: HYG Database v4.1, Astronexus (github.com/astronexus/HYG-Database). Fields derived from it stay under CC BY-SA 4.0.
The stellar parameters marked as a Gaia DR3 model fit were taken from Gaia DR3 astrophysical parameters (GSP-Phot and FLAME), credit ESA/Gaia/DPAC, under CC BY-NC 3.0 IGO. ESA’s terms and requested acknowledgement: Credit: ESA/Gaia/DPAC. Licence: CC BY-NC 3.0 IGO, https://creativecommons.org/licenses/by-nc/3.0/igo/, non-commercial use only; commercial use needs ESA's prior authorisation. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Cite Gaia Collaboration 2016, A&A 595, A1 (2016A&A...595A...1G) and Gaia Collaboration 2023, A&A 674, A1 (2023A&A...674A...1G).