View source for Hungaria family

{{About|the collisional asteroid family|the dynamical group this family is part of|Hungaria asteroid}}

The '''Hungaria family''' ([[Asteroid family#003|003]]<ref name="Nesvorny2015">{{cite journal |last1=Nesvorny |first1=D. |last2=Broz |first2=M. |last3=Carruba |first3=V. |title=Identification and Dynamical Properties of Asteroid Families |date=2015 |arxiv=1502.01628 |journal=Asteroids IV |doi=10.2458/azu_uapress_9780816532131-ch016 |isbn=978-0-8165-3213-1 }}</ref>) is a collisional [[asteroid family]] of at least 2,966 known asteroids,<ref name="Nesvorny2020">{{cite book |last1=Nesvorný |first1=David |title= Nesvorny HCM Asteroid Families Bundle V1.0|chapter=Asteroids |date=14 August 2020 |publisher=NASA Planetary Data System |doi=10.26033/6cg5-pt13}}</ref> named for its largest member, the {{convert|11|km|mi|adj=on}}-across asteroid [[434 Hungaria]]. It lies within the larger dynamical group of [[Hungaria asteroid]]s, a group of asteroids in the far inner [[asteroid belt]], with [[Semi-major and semi-minor axes|semimajor axes]] of 1.78 to 2.00 [[astronomical unit|AU]]. All members of the family are bright [[E-type asteroid]]s with [[albedo]]s of around 0.35-0.6.

An asteroid family is a group of physically-related asteroids usually created by a collision with an original larger asteroid, with the fragments continuing on similar orbits to the original. This is distinct from a [[List of minor-planet groups#Other groups out to the orbit of Jupiter|dynamical group]] in that the members of a dynamical group only share similar orbits because of gravitational interactions with planets, which concentrate asteroids in a particular orbital range. Members of the Hungaria family are both part of the wider [[Hungaria asteroid|Hungaria dynamical group]], and fragments of 434 Hungaria. The family is considered a catastrophic asteroid family because 434 Hungaria, its largest member, makes up only a fifth of the family's mass.<ref>{{cite journal |last1=Holsapple |first1=K.A. |last2=Housen |first2=K.R. |title=The catastrophic disruptions of asteroids: History, features, new constraints and interpretations |journal=Planetary and Space Science |date=December 2019 |volume=179 |pages=104724 |doi=10.1016/j.pss.2019.104724 |url=https://www.sciencedirect.com/science/article/abs/pii/S0032063319300509 |access-date=30 July 2024}}</ref>

The family has been variously estimated to be {{val|205|45}} million years,<ref>{{cite web |title=Asteroid Family Ages |url=https://newton.spacedys.com/astdys/fam_ages/ |website=AstDyS |access-date=28 July 2024}}</ref> 275 million years,<ref>{{cite journal |last1=Lucas |first1=Michael P. |last2=Emery |first2=Joshua P. |last3=MacLennan |first3=Eric M. |last4=Pinilla-Alonso |first4=Noemi |last5=Cartwright |first5=Richard J. |last6=Lindsay |first6=Sean S. |last7=Reddy |first7=Vishnu |last8=Sanchez |first8=Juan A. |last9=Thomas |first9=Cristina A. |last10=Lorenzi |first10=Vania |title=Hungaria asteroid region telescopic spectral survey (HARTSS) II: Spectral homogeneity among Hungaria family asteroids |journal=Icarus |date=April 2019 |volume=322 |pages=227–250 |doi=10.1016/j.icarus.2018.12.010 |bibcode=2019Icar..322..227L |url=https://ui.adsabs.harvard.edu/abs/2019Icar..322..227L/abstract |access-date=30 July 2024}}</ref> and {{val|400|100}} million years old.<ref>{{cite journal |last1=Forgács-Dajka |first1=E. |last2=Sándor |first2=Zs |last3=Sztakovics |first3=J. |title=A survey on Hungaria asteroids involved in mean motion resonances with Mars |journal=Astronomy & Astrophysics |date=1 January 2022 |volume=657 |pages=A135 |doi=10.1051/0004-6361/202141719|arxiv=2110.11745 }}</ref>

==Large members==

{{Image frame
 |width = 252
 |align = right
 |pos = bottom
 |content =<div style="background-color: #F9F9F9; font-size: 0.85em; text-align: left; padding: 8px 0; margin: 0;">
 {{#invoke:Chart
  |pie chart
  |radius = 125
  |slices = 
    ( 0.0147 : [[434 Hungaria]] :: [[434 Hungaria]])
    ( 0.00384 : [[1103 Sequoia]] :: [[1103 Sequoia]])
    ( 0.00157 : [[3169 Ostro]] :: [[3169 Ostro]])
    ( 0.000889 : [[4031 Mueller]] :: [[4031 Mueller]])
    ( 0.000693 : [[3086 Kalbaugh]] :: [[3086 Kalbaugh]])
    ( 0.000579 : [[1919 Clemence]] :: [[1919 Clemence]])
    ( 0.000519 : [[5390 Huichiming]] :: [[5390 Huichiming]])
    ( 0.000464 : [[5427 Jensmartin]] :: [[5427 Jensmartin]])
    ( 0.000439 : [[4232 Aparicio]] :: [[4232 Aparicio]])
    ( 0.000421 : [[5378 Ellyett]] :: [[5378 Ellyett]])
    ( 0.0541 : all other members :: [[Hungaria family]])
  |units suffix = <!--calculated using an arbitrary density of 2 g/cm^3. the absolute mass values are irrelevant as these are being measured relatively-->
  |percent = true
  }}</div>
 |caption= Mass distribution of the Schubart family (assuming similar densities)
}}

{| class="wikitable sortable"
|+The 10 brightest Hungaria family members<ref name="Nesvorny2020"/>
|-
!Name !! [[absolute magnitude|Abs. Mag]] !! Size (km) !! [[Semi-major and semi-minor axes|proper<br/>a]] ([[astronomical unit|AU]]) !! [[orbital eccentricity|proper<br/>e]] !! [[orbital inclination|proper<br/>i]]
|-
|[[434 Hungaria]] || 11.24 || 11 || 1.9443 || 0.078 || 20.868
|-
|[[1103 Sequoia]] || 12.21 || 6.7 || 1.9336 || 0.083 || 20.847
|-
|[[3169 Ostro]] || 12.86 || 4.7 || 1.8918 || 0.070 || 22.357
|-
|[[4031 Mueller]] || 13.27 || 3.9 || 1.9342 || 0.071 || 20.624
|-
|[[3086 Kalbaugh]] || 13.45 || 4.0 || 1.9358 || 0.048 || 21.800
|-
|[[1919 Clemence]] || 13.58 || 3.3 || 1.9360 || 0.075 || 20.980
|-
|[[5390 Huichiming]] || 13.66 || 3.4 || 1.9391 || 0.059 || 21.111
|-
|[[5427 Jensmartin]] || 13.74 || 3.2 || 1.9317 || 0.085 || 21.162
|-
|[[4232 Aparicio]] || 13.78 || 3.3 || 1.9362 || 0.063 || 20.608
|-
|[[5378 Ellyett]] || 13.81 || 3.0 || 1.9342 || 0.073 || 21.213
|}

==References==
{{reflist}}

[[Category:Hungaria asteroids|*]]
[[Category:Asteroid groups and families]]