Draft:ASASSN-24fw
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ASASSN-24fw is a F-type main-sequence star that underwent a rare, prolonged occultation event detected by the All Sky Automated Survey for SuperNovae (ASAS-SN), resulting in a deep dimming of approximately 4.1 magnitudes in the g-band lasting about 8–9 months from late September 2024 to late May or June 2025.[5][6]
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Comment: That's why i completely overhauled the article Abdullah1099 (talk) 04:22, 6 March 2026 (UTC)
- Comment: very interesting. this objetcs has been widely covered by the media. it would be great to some see some more secondary sources. Astropedian (talk) 12:35, 5 March 2026 (UTC)
 | This is a draft article. It is a work in progress open to editing by anyone. Please ensure core content policies are met before publishing it as a live Wikipedia article. Find sources: Google (books · news · scholar · free images · WP refs) · FENS · JSTOR · TWL Last edited by Abdullah1099 (talk | contribs) 14 days ago. (Update)
This draft has been submitted and is currently awaiting review. |
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| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Monoceros |
| Right ascension | 07h 51m 41.996s[1] |
| Declination | +09° 23′ 9.79″[1] |
| Characteristics | |
| Evolutionary stage | Main-sequence |
| Spectral type | F8IV[2] |
| Astrometry | |
| Radial velocity (Rv) | 36.87 [3] km/s |
| Proper motion (μ) | RA: -3.75[3] mas/yr Dec.: -7.612[3] mas/yr |
| Distance | 3,260[4] ly |
| Details[4][2] | |
| Mass | 1.40+0.07 −0.11 M☉ |
| Radius | 1.95+0.05 −0.06 R☉ |
| Age | 2.75 ± 0.24 Gyr |
| Other designations | |
| ASASSN-24fw, 2MASS J07051897+0612195, WISE J070518.97+061219.5, UCAC4 482-031200, Gaia DR3 3152916838954800512[3] | |
| Database references | |
| SIMBAD | data |
Observation
The star is located approximately 3,260 light-years away in the constellation of Monoceros. It has an estimated mass of about 1.4 M☉ and exhibits an infrared excess indicative of circumstellar dust, with pre-event photometry showing stability over more than a decade of ASAS-SN monitoring.[4]
One model attributes the occultation to optically thick rings or a circumplanetary disk surrounding either a red dwarf[7] or a substellar companion[8][9] (brown dwarf or massive gas giant, minimum mass around 3–3.4 MJ), with ring radius ~0.17 AU forming a large structure at ~14 AU orbital separation.[4][10]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (years) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| Ab (unconfirmed) | 3.4 MJ | 14.0 | 16060.0 | 0.88±0.07 | — | — |