HH 30

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HH 30
HH 30.jpg
HH 30 with Hubble ACS
Credit: ESA/Hubble and NASA Acknowledgement: Judy Schmidt
Observation data
Epoch J2000       Equinox J2000
Constellation Taurus
Right ascension 04h 31m 37.51s
Declination +18° 12′ 24.38″
Apparent magnitude  (V)18.50 ±0.31 [1]
Characteristics
Evolutionary stage T Tauri star [2]
Spectral type M0 ±2 [3]
Variable type variable nebula [4]
Astrometry
Radial velocity (Rv)20.3 ±3.5 [3]  km/s
Distance 146.4 ±0.5  pc [2]
Details
Mass 0.45 ±0.14 [5]   M☉
Temperature 3700 [3]   K
Rotational velocity (v sin i)≤12 [3]  km/s
Age approx. 1–2 [6]   Myr
Other designations
2MASS  J04313747+1812244, JCMTSF  J043137.4+181226, HH 30, HH 30 IRS, V1213 Tau, WISE  J043137.48+181224.2, EPIC  210689083, TIC  353752582, Gaia  DR3 3314311981834278912
Database references
SIMBAD data

HH-30 (also V1213 Tauri) is an edge-on protoplanetary disk that is surrounded by jets and a disk wind. [6] HH-30 is located in the dark cloud LDN 1551 in the Taurus Molecular Cloud. The HH-30 disk is the prototype of an edge-on disk, [2] due to its early discovery with Hubble. [4]

Contents

Discovery

HH 30 was published by George Herbig in 1974 in the "Draft Catalog of Herbig–Haro Objects" and notes: "HH-30 (4h 28m 44s) is a small, almost stellar spot 2' south of XZ and HL Tau. There is a fainter nebulosity immediately northeast. The small fuzzy spot of very similar appearance at 35" in 250° from HL Tau is not a HH Object, but a star having Hα in emission." [7] In 1996 it became clear that the object is an edge-on protoplanetary disk with jets. [4]

The central star

The star is hidden behind the dust of the disk. The spectral type was measured around M0 with the Keck Observatory, corresponding to a temperature of around 3700 Kelvin. [3] Disk rotation constrained the star mass to 0.45 M☉. [8] [5] One study suggest that the central object is a binary star, due to the jet wiggling. [9] A follow-up study found that the jet-producing primary has a mass of 0.31 ±0.04 M☉ and that the secondary has a mass of 0.14 ±0.03 M☉. Both objects should be separated by 18.0 ±0.6 astronomical units (AU). [10]

Protoplanetary disk

Observations with Hubble WFPC2 in 1996 discovered the disk, which has a radius of 250 AU. The disk is seen as a bi-reflection nebula and the disk blocks the light of the star. The northern part of the reflection nebula decreased in brightness by 0.5 mag between two observations, while the southern part increased in brightness by 0.5 mag. [4] The disk around the star is a class II disk, meaning it contains both gas and dust particles. [3] Observations with the Plateau de Bure interferometer detected the carbon monoxide (CO) emission and measured the rotation of the disk. [8] Observations with the Atacama Large Millimeter Array (ALMA) showed the mid-plane of the disk in 13CO and also measured its rotation. [5] A study with JWST and archived Hubble and ALMA data was published in 2024. This showed inefficient dust settling in the disk. Dust settling means that larger dust grains settle to the mid-plane of the disk. The observation also showed that the disk contains spiral-like and tail-like structure. The disk has a very high inclination of at least 84°. [2]

Jets

The jets were discovered in 1983 from CCD images at Calar Alto Observatory. [11] A proper motion survey in 1990 showed a speed of around 170 km/s of the jets. This study also detected H-alpha, ionized nitrogen and sulfur in the jet. [12] Early observations with Hubble showed that the knots of the jet have a speed of 100 to 300 km/s. [4] JWST NIRCam and MIRI observations showed the previously observed jet and a bi-conical outflow. The jet is bright in the MIRI F1280W filter, likely tracing ionized neon emission. One knot was seen moving with around 121 km/s. [2] The jet is seen with NIRSpec in ionized iron with a tight semi-opening angle of 1.4°±0.9°. [6]

Disk wind

A CO outflow was first resolved in 2006, [8] and in 2024 the outflow was detected with ALMA in 12CO. The researchers found three distinct shells in the outflow and measured an outflow mass of (1.83 ±0.19)×10‑4M☉. This outflow is expanding with a speed of around 4–6 km/s and possibly rotates with a speed of ≤0.5 km/s. These shells can be explained by a magnetocentrifugal disk winds (MHD wind). [5] Another study using NIRSpec and ALMA, found that the outflow is nestled within each other. The jet is seen with a tight semi-opening angle of around 1.4°. The disk wind is seen with a wider semi-opening angle, with the molecular hydrogen (H2) emission having a semi-opening angle of around 14°. But this emission is also nestled within cold carbon monoxide (CO) emission from ALMA. [6]

See also

examples of other edge-on disks

Related Research Articles

<span class="mw-page-title-main">Protoplanetary disk</span> Gas and dust surrounding a newly formed star

A protoplanetary disk is a rotating circumstellar disc of dense gas and dust surrounding a young newly formed star, a T Tauri star, or Herbig Ae/Be star. The protoplanetary disk may not be considered an accretion disk; while the two are similar, an accretion disk is hotter and spins much faster. It is also found on black holes, not stars. This process should not be confused with the accretion process thought to build up the planets themselves. Externally illuminated photo-evaporating protoplanetary disks are called proplyds.

<span class="mw-page-title-main">Proplyd</span> Dust ring surrounding large stars thousands of solar radii wide

A proplyd, short for ionized protoplanetary disk, is an externally illuminated photoevaporating protoplanetary disk around a young star. Nearly 180 proplyds have been discovered in the Orion Nebula. Images of proplyds in other star-forming regions are rare, while Orion is the only region with a large known sample due to its relative proximity to Earth.

<span class="mw-page-title-main">T Tauri</span> Star in constellation Taurus

T Tauri is a trinary variable star in the constellation Taurus, the prototype of the T Tauri stars. It was discovered in October 1852 by John Russell Hind. T Tauri appears from Earth amongst the Hyades cluster, not far from ε Tauri, but it is actually 420 light-years behind it and not a member of the cluster. The cloud to the west of the system is NGC 1555, known more commonly as Hind's Variable Nebula.

<span class="mw-page-title-main">2M1207</span> Brown dwarf in the constellation Centaurus

2M1207, 2M1207A or 2MASS J12073346–3932539 is a brown dwarf located in the constellation Centaurus; a companion object, 2M1207b, may be the first extrasolar planetary-mass companion to be directly imaged, and is the first discovered orbiting a brown dwarf.

<span class="mw-page-title-main">Herbig–Haro object</span> Small patches of nebulosity associated with newly born stars

Herbig–Haro (HH) objects are bright patches of nebulosity associated with newborn stars. They are formed when narrow jets of partially ionised gas ejected by stars collide with nearby clouds of gas and dust at several hundred kilometers per second. Herbig–Haro objects are commonly found in star-forming regions, and several are often seen around a single star, aligned with its rotational axis. Most of them lie within about one parsec of the source, although some have been observed several parsecs away. HH objects are transient phenomena that last around a few tens of thousands of years. They can change visibly over timescales of a few years as they move rapidly away from their parent star into the gas clouds of interstellar space. Hubble Space Telescope observations have revealed the complex evolution of HH objects over the period of a few years, as parts of the nebula fade while others brighten as they collide with the clumpy material of the interstellar medium.

<span class="mw-page-title-main">Bipolar outflow</span> Two continuous flows of gas from the poles of a star

A bipolar outflow comprises two continuous flows of gas from the poles of a star. Bipolar outflows may be associated with protostars, or with evolved post-AGB stars.

<span class="mw-page-title-main">HH 46/47</span> Herbig-Haro objects in the constellation Vela

HH 46/47 is a complex of Herbig–Haro objects, located around 450 parsecs away in a Bok globule near the Gum nebula. Jets of partially ionized gas emerging from a young star produce visible shocks upon impact with the ambient medium. Discovered in 1977, it is one of the most studied HH objects and the first jet to be associated with young stars was found in HH 46/47. Four emission nebulae, HH 46, HH 47A, HH 47C and HH 47D and a jet, HH 47B, have been identified in the complex. It also contains a mostly unipolar molecular outflow, and two large bow shocks on opposite sides of the source star. The overall size of the complex is about 3 parsecs.

<span class="mw-page-title-main">NGC 1333</span> Reflection nebula in the constellation Perseus

NGC 1333 is a reflection nebula located in the northern constellation Perseus, positioned next to the southern constellation border with Taurus and Aries. It was first discovered by German astronomer Eduard Schönfeld in 1855. The nebula is visible as a hazy patch in a small telescope, while a larger aperture will show a pair of dark nebulae designated Barnard 1 and Barnard 2. It is associated with a dark cloud L1450. Estimates of the distance to this nebula range from 980–1,140 ly (300–350 pc).

<span class="mw-page-title-main">AB Aurigae</span> Star in the constellation Auriga

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<span class="mw-page-title-main">HL Tauri</span> Star in constellation Taurus

HL Tauri is a young T Tauri star in the constellation Taurus, approximately 450 light-years (140 pc) from Earth in the Taurus Molecular Cloud. The luminosity and effective temperature of HL Tauri imply that its age is less than 100,000 years. At apparent magnitude 15.1, it is too faint to be seen with the unaided eye. It is surrounded by a protoplanetary disk marked by dark bands visible in submillimeter radiation that may indicate a number of planets in the process of formation. It is accompanied by the Herbig–Haro object HH 150, a jet of gas emitted along the rotational axis of the disk that is colliding with nearby interstellar dust and gas.

<span class="mw-page-title-main">RCW 36</span> Emission nebula in the constellation of Vela

RCW 36 is an emission nebula containing an open cluster in the constellation Vela. This H II region is part of a larger-scale star-forming complex known as the Vela Molecular Ridge (VMR), a collection of molecular clouds in the Milky Way that contain multiple sites of ongoing star-formation activity. The VMR is made up of several distinct clouds, and RCW 36 is embedded in the VMR Cloud C.

<span class="mw-page-title-main">HD 169142</span> Pre-main-sequence star in the constellation Sagittarius

HD 169142 is a single Herbig Ae/Be star. Its surface temperature is 7650±150 K. HD 169142 is depleted of heavy elements compared to the Sun, with a metallicity Fe/H index of −0.375±0.125, but is much younger at an age of 7.5±4.5 million years. The star is rotating slowly and has relatively low stellar activity for a Herbig Ae/Be star.

<span class="mw-page-title-main">PDS 70</span> T Tauri-type star in the constellation Centaurus

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<span class="mw-page-title-main">Circumplanetary disk</span> Accumulation of matter around a planet

A circumplanetary disk is a torus, pancake or ring-shaped accumulation of matter composed of gas, dust, planetesimals, asteroids or collision fragments in orbit around a planet. They are reservoirs of material out of which moons may form. Such a disk can manifest itself in various ways.

<span class="mw-page-title-main">HH 1/2</span> Herbig-Haro object in the constellation Orion

The Herbig-Haro objects HH 1/2 are the first such objects to be recognized as Herbig-Haro objects and were discovered by George Herbig and Guillermo Haro. They are located at a distance of about 1343 light-years in the constellation Orion near NGC 1999. HH 1/2 are among the brightest Herbig-Haro objects in the sky and consist of a pair of oppositely oriented bow shocks, separated by 2.5 arcminutes. The HH 1/2 pair were the first Herbig-Haro objects with detected proper motion and HH 2 was the first Herbig-Haro object to be detected in x-rays. Some of the structures in the Herbig-Haro Objects move with a speed of 400 km/s.

<span class="mw-page-title-main">HD 163296</span> HD 163296 is a Herbig Ae star

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<span class="mw-page-title-main">Proplyd 114-426</span> Proplyd 114-426 is a protoplanetary disk

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<span class="mw-page-title-main">IC 5063</span> Galaxy in the constellation Indus

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<span class="mw-page-title-main">2MASS J04202144+2813491</span> 2MASS J04202144+2813491 is a protoplanetary disk in Taurus

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References

  1. ↑ Lasker, Barry M.; Lattanzi, Mario G.; McLean, Brian J.; Bucciarelli, Beatrice; Drimmel, Ronald; Garcia, Jorge; Greene, Gretchen; Guglielmetti, Fabrizia; Hanley, Christopher; Hawkins, George; Laidler, Victoria G.; Loomis, Charles; Meakes, Michael; Mignani, Roberto; Morbidelli, Roberto (2008-08-01). "The Second-Generation Guide Star Catalog: Description and Properties". The Astronomical Journal. 136 (2): 735–766. arXiv: 0807.2522 . Bibcode:2008AJ....136..735L. doi:10.1088/0004-6256/136/2/735. ISSN   0004-6256.
  2. 1 2 3 4 5 Tazaki, Ryo; Ménard, François; Duchêne, Gaspard; Villenave, Marion; Ribas, Álvaro; Stapelfeldt, Karl R.; Perrin, Marshall D.; Pinte, Christophe; Wolff, Schuyler G. (2024-12-01). "JWST Imaging of Edge-on Protoplanetary Disks. IV. Mid-infrared Dust Scattering in the HH 30 disk". arXiv: 2412.07523 [astro-ph].
  3. 1 2 3 4 5 6 White, Russel J.; Hillenbrand, Lynne A. (2004-12-01). "On the Evolutionary Status of Class I Stars and Herbig-Haro Energy Sources in Taurus-Auriga". The Astrophysical Journal. 616 (2): 998–1032. arXiv: astro-ph/0408244 . Bibcode:2004ApJ...616..998W. doi:10.1086/425115. ISSN   0004-637X.
  4. 1 2 3 4 5 Burrows, Christopher J.; Stapelfeldt, Karl R.; Watson, Alan M.; Krist, John E.; Ballester, Gilda E.; Clarke, John T.; Crisp, David; Gallagher, John S., III; Griffiths, Richard E.; Hester, J. Jeff; Hoessel, John G.; Holtzman, Jon A.; Mould, Jeremy R.; Scowen, Paul A.; Trauger, John T. (1996-12-01). "Hubble Space Telescope Observations of the Disk and Jet of HH 30". The Astrophysical Journal. 473: 437–451. Bibcode:1996ApJ...473..437B. doi:10.1086/178156. ISSN   0004-637X.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  5. 1 2 3 4 López-Vázquez, J. A.; Lee, Chin-Fei; Fernández-López, M.; Louvet, Fabien; Guerra-Alvarado, O.; Zapata, Luis A. (2024-02-01). "Multiple Shells Driven by Disk Winds: ALMA Observations in the HH 30 Outflow". The Astrophysical Journal. 962 (1): 28. arXiv: 2312.03272 . Bibcode:2024ApJ...962...28L. doi: 10.3847/1538-4357/ad132a . ISSN   0004-637X.
  6. 1 2 3 4 Pascucci, Ilaria; Beck, Tracy L.; Cabrit, Sylvie; Bajaj, Naman S.; Edwards, Suzan; Louvet, Fabien; Najita, Joan R.; Skinner, Bennett N.; Gorti, Uma; Salyk, Colette; Brittain, Sean D.; Krijt, Sebastiaan; Muzerolle Page, James; Ruaud, Maxime; Schwarz, Kamber (2024-10-01). "The nested morphology of disk winds from young stars revealed by JWST/NIRSpec observations". Nature Astronomy. 9: 81–89. arXiv: 2410.18033 . Bibcode:2024NatAs.tmp..279P. doi:10.1038/s41550-024-02385-7. ISSN   2397-3366.{{cite journal}}: CS1 maint: bibcode (link)
  7. ↑ Herbig, G. H. (1974-01-01). "Draft Catalog of Herbig-Haro Objects". Lick Observatory Bulletin. 658: 1. Bibcode:1974LicOB.658....1H. ISSN   0075-9317.
  8. 1 2 3 Pety, J.; Gueth, F.; Guilloteau, S.; Dutrey, A. (2006-11-01). "Plateau de Bure interferometer observations of the disk and outflow of HH 30". Astronomy and Astrophysics. 458 (3): 841–854. arXiv: astro-ph/0608218 . Bibcode:2006A&A...458..841P. doi:10.1051/0004-6361:20065814. ISSN   0004-6361.
  9. ↑ Anglada, Guillem; López, Rosario; Estalella, Robert; Masegosa, Josefa; Riera, Angels; Raga, Alejandro C. (2007-06-01). "Proper Motions of the Jets in the Region of HH 30 and HL/XZ Tau: Evidence for a Binary Exciting Source of the HH 30 Jet". The Astronomical Journal. 133 (6): 2799–2814. arXiv: astro-ph/0703155 . Bibcode:2007AJ....133.2799A. doi:10.1086/517493. ISSN   0004-6256.
  10. ↑ Estalella, Robert; López, Rosario; Anglada, Guillem; Gómez, Gabriel; Riera, Angels; Carrasco-González, Carlos (2012-08-01). "The Counterjet of HH 30: New Light on Its Binary Driving Source". The Astronomical Journal. 144 (2): 61. arXiv: 1206.3391 . Bibcode:2012AJ....144...61E. doi:10.1088/0004-6256/144/2/61. ISSN   0004-6256.
  11. ↑ Mundt, R.; Fried, J. W. (1983-11-01). "Jets from young stars". The Astrophysical Journal. 274: L83 –L86. Bibcode:1983ApJ...274L..83M. doi:10.1086/184155. ISSN   0004-637X.
  12. ↑ Mundt, R.; Buehrke, T.; Solf, J.; Ray, T. P.; Raga, A. C. (1990-06-01). "Optical jets and outflows in the HL Tauri region". Astronomy and Astrophysics. 232: 37. Bibcode:1990A&A...232...37M. ISSN   0004-6361.
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