恆星由分子雲形成,為宇宙最基本的組成份子。恆星形成的過程改變了分子雲的物理及化學環境,因此不僅控制了星系的結構和演化,也掌控了重元素逐步生成,及讓生命得以產生的行星環境。在如此的動力過程中,分子雲收縮產生了分子雲核,進而因重力坍縮形成年輕星體,接下來經由拱星盤發生物質吸積,這又伴隨著如恆星風,噴流或外向流導致物質流失,最終分子雲包層潰散。這只是我們所了解恆星形成的約略過程,但其細節尙未完全了解,故仍為現代天文學中的主要研究課題。本所恆星形成研究小組致力於以理論模型及觀測上的證據來了解恆形形成過程的本質。
How the protoplanetary disk forms around the young star L1527 IRS: ALMA discovers the “ENDTRANZ” Missing Link
The [Ne III] Jet of DG Tau and Its Ionization Scenarios
A study of the wiggle morphology of HH 211 through numerical simulations: View of the simulation
A study of the wiggle morphology of HH 211 through numerical simulations
ALMA revealed the earliest stage of protostellar evolution
An extremely young protostar, SMM11, observed in millimeter wavelength
Visibility distribution of the protostar L1527 IRS in 220 GHz continuum
How a supernova affects a nearby star-forming galaxy?
Is FS Tau B Driving an Asymmetric Jet?
Velocity-Resolved [Ne III] from X-ray Irradiated Sz 102 Microjets
ALMA Observation of Gas Spirals as a Nursery of Binary Stars
Dust distribution in the binary protostellar system L1551 NE observed with the SMA in 0.9 mm continuum.
Infalling Flow toward a Keplerian Disk around the Protostar L1489 IRS
Infalling and Rotational Motions of Ambient Gas around 17 Protostars
A still-forming protostar which is accreting material from a surrounding disk
Two submm sources in the B1-b molecular cloud core.
Youngest Protoplanetary Disk Discovered with ALMA
A rotating disk (from the SMA observations) is detected around a protostar launching a powerful jet in Orion
First detection of HC3N in protoplanetary disks
a layer of dust almost transparent in the near infrared sitting above the protoplanetary disk around RY Tau star