Parshati Patel

Social Media Prize by IAU

2019-01-29

Parshati was awarded a Social Media prize (a certificate and a telescope) by International Astronomical Union for outstanding contributions for popularizing the events on social media during the 100 Hours of Astronomy Campaign in January 2019. Parshati talked to various universities, organizations and members of the public during the 100 Hours of Astronomy Campaign.

Gujarat Gaurav (Pride of Gujarat) Award - Female

2019-04-30

Parshati was awarded the Gujarat Gaurav (Pride of Gujarat) award in the Female category by Gujarat Public Affairs Council of Canada for outstanding contributions to Outreach and Research as a Gujarati in Canada in May 2019 in Toronto, Ontario, Canada.

Award of Excellence - Operations

2019-02-28

Parshati proposed and led the Western University’s Space Explorers Program at the historic David Dunlap Observatory in Richmond Hill, Ontario, Canada, in partnership with The Town of Richmond Hill. The town of Richmond Hill and the partner organizations (including Western University) were awarded for unique programs, activities and events at David Dunlap Observatory in March 2019 by Parks and Recreation Ontario.

Western University

Master the Entrepreneur Skillset

Entrepreneurship/ Entrepreneurial Studies

2020

Grade: Certificate of Achievement
The Master the Entrepreneur Skillset is a 6-Week Virtual Masterclass Powered by Western Entrepreneurship and Ivey Business School to help Western alumni, students, faculty and staff restart economies and create jobs.

Western University

Professional Certificate

Communications and Public Relations

2021

Western University

Certificate

Digital Communications

2021

Photoionization Models for the Inner Gaseous Disks of Herbig Be Stars: Evidence Against Magnetospheric Accretion?

2017-01-24

We investigate the physical properties of the inner gaseous disks of the three, hot, Herbig B2e stars, HD 76534, HD 114981 and HD 216629, by modelling CFHT-ESPaDOns spectra using non-LTE radiative transfer codes. We assume that the emission lines are produced in a circumstellar disk heated solely by the photospheric radiation from the central star in order to test if the optical and near-IR emission lines can be reproduced without invoking magnetospheric accretion. The inner gaseous disk density was assumed to follow a simple power-law in the equatorial plane, and we searched for models that could reproduce observed lines of HI (Hα and Hβ), HeI, CaII and FeII. For the three stars, good matches were found for all emission line profiles individually; however, no density model based on a single power-law was able to reproduce all of the observed emission lines. Among the single power-law models, the one with the gas density varying as ~10^{-10}(R*/R)^3 g/cm^3 in the equatorial plane of a 25R* (0.78 AU) disk did the best overall job of representing the optical emission lines of the three stars. This model implies a mass for the Hα-emitting portion of the inner gaseous disk of ~10^{-9} M*. We conclude that the optical emission line spectra of these HBe stars can be qualitatively reproduced by a ~1 AU, geometrically thin, circumstellar disk of negligible mass compared to the central star in Keplerian rotation and radiative equilibrium.

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Photoionization Models of the Inner Gaseous Disk of the Herbig Be Star BD+65 1637

2016-01-01

We attempt to constrain the physical properties of the inner, gaseous disk of the Herbig Be star BD+65 1637 using non-LTE, circumstellar disk codes and observed spectra (3700-10500 Å) from the ESPaDOnS instrument on the Canada-France-Hawaii Telescope. The photoionizing radiation of the central star is assumed to be the sole source of input energy for the disk. We model optical and near-infrared emission lines that are thought to form in this region using standard techniques that have been successful in modeling the spectra of classical Be stars. By comparing synthetic line profiles of hydrogen, helium, iron, and calcium with the observed line profiles, we try to constrain the geometry, density structure, and kinematics of the gaseous disk. Reasonable matches have been found for all line profiles individually; however, no disk density model based on a single power law for the equatorial density was able to simultaneously fit all of the observed emission lines. Among the emission lines, the metal lines, especially the Ca ii IR triplet, seem to require higher disk densities than the other lines. Excluding the Ca ii lines, a model in which the equatorial disk density falls as 10-10 (R*/R)3 g cm-3 seen at an inclination of 45° for a 50 R* disk provides reasonable matches to the overall line shapes and strengths. The Ca ii lines seem to require a shallower drop-off as 10-10 (R*/R)2 g cm-3 to match their strength. More complex disk density models are likely required to refine the match to the BD+65 1637 spectrum.

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The Correlation between Hα Emission and Visual Magnitude during Long-term Variations in Classical Be Stars

2013-03-01

Hα equivalent widths and UBV magnitudes are calculated for Be star disk models that grow in size and/or density with time. We show that these simple models are consistent with the known Be star classes of positive and inverse correlations between long-term variations in Hα and V magnitude as identified by Harmanec. We support the conclusion of Harmanec that the distinction is controlled by the inclination of the disk to the line of sight. We demonstrate that the strength of these correlations, particularly those of an inverse correlation where the system becomes fainter as the Hα emission strength grows, is strongly influenced by the scale height of the inner Be star disk and the extent of the gravitational darkening of the central B star due to rapid rotation. This dependence may allow coordinated spectroscopic and photometric observations to better constrain these poorly known Be star parameters.

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